IRAM Annual Report 2012

Transcription

IRAM
6 x 15-meter interferometer, Plateau de Bure
Institut de Radioastronomie Millimétrique 30-meter diameter telescope, Pico Veleta
The Institut de Radioastronomie Millimétrique (IRAM) is a multi-national
scientific institute covering all aspects of radio astronomy at millimeter
wavelengths: the operation of two high-altitude observatories – a
30-meter diameter telescope on Pico Veleta in the Sierra Nevada (southern
Spain), and an interferometer of six 15 meter diameter telescopes on the
Plateau de Bure in the French Alps – the development of telescopes and
instrumentation, radio astronomical observations and their interpretation.
IRAM Addresses:
Institut de Radioastronomie
Millimétrique
300 rue de la piscine,
Saint-Martin d’Hères
F-38406 France
Tel: +33 [0]4 76 82 49 00
Fax: +33 [0]4 76 51 59 38
[email protected] www.iram.fr
Observatoire
du Plateau de Bure
Saint-Etienne-en-Dévoluy
F-05250 France
Tel: +33 [0]4 92 52 53 60
Fax: +33 [0]4 92 52 53 61
Avenida Divina Pastora 7, Local 20,
E-18012 Granada, España
Tel: +34 958 80 54 54
Fax: +34 958 22 23 63
[email protected]
Observatorio
Radioastronómico
de Pico Veleta
Sierra Nevada,
Granada, España
Tel: +34 958 48 20 02
Fax: +34 958 48 11 49
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The technical and scientific staff of IRAM develops instrumentation and
software for the specific needs of millimeter radioastronomy and for the
benefit of the astronomical community. IRAM’s laboratories also supply
devices to several European partners, including for the ALMA project.
IRAM’s scientists conduct forefront research in several domains of
astrophysics, from nearby star-forming regions to objects at cosmological
distances.
IRAM Partner Organizations:
Centre National de la Recherche Scientifique (CNRS) – Paris, France
Max-Planck-Gesellschaft (MPG) – München, Deutschland
Instituto Geografico Nacional (IGN) – Madrid, España
Annual Report 2012
Instituto de Radioastronomía
Milimétrica
IRAM was founded in 1979 by two national research organizations: the
CNRS and the Max-Planck-Gesellschaft – the Spanish Instituto Geográfico
Nacional, initially an associate member, became a full member in 1990.
Front Cover
Cas A as seen in the 2mm
wavelength band by NIKA (NEEL
IRAM KID ARRAY), the prototype
continuum camera at the 30m
telescope using lumped Element
Kinetic Inductance Detectors. The
emission from Cas A, a well known
supernova remnant, is dominated in
this band by synchrotron radiation.
Annual report 2012
Published by IRAM © 2013
Director of publication Karl-Friedrich Schuster
With contributions from:
Sébastien Blanchet, Michael Bremer, Walter Brunswig, Isabelle Delaunay,
Frédéric Gueth, Carsten Kramer, Bastien Lefranc, Alessandro Navarrini,
Santiago Navarro, Roberto Neri, Juan Penalver, Marc Torres
1
Annual report 2012
Contents
Introduction5
Highlights of research with the IRAM telescopes in 2012
6
The observatories
15
The 30-meter telescope
15
Plateau de Bure interferometer
21
Grenoble Headquarters
26
Frontend group
26
SIS group
37
Backend group
38
Mechanical group
38
Computer group
41
Science software activities
42
IRAM ARC Node
44
Personnel and finances
46
Annexes48
Annex I – Telescope schedules
48
Annex II – Publications in 2012
58
Annex III – Committee members
67
3
Annual report 2012
Introduction
2012 has been a pivotal year for IRAM with
many important steps taken for the future. Most
importantly NOEMA, the Northern Extended
Millimeter Array Project started its transition
from a mere concept to reality with important
supplier contracts already signed, a well-advanced
technology development and the organizational
scheme well in place. Many details of the ongoing
work for NOEMA can be found in this annual report.
Current planning foresees first light for the first
NOEMA antenna in spring 2014.
In parallel to NOEMA, the construction of the new
cable car for an improved access to the Plateau de
Bure has finally started this year and operation is
also foreseen for early 2014. The two simultaneous
projects, NOEMA and cable car construction, require
a particular level of organization at the Plateau de
Bure site, a real challenge to all participants in these
projects. We are confident that with the detailed
planning in place, this challenge can be met.
Meanwhile IRAM has continued to produce
outstanding science with both observatories. At
the IRAM 30m telescope, EMIR, the most powerful
operating millimeter wave receiver, has allowed us to
make a quantum leap in frequency surveys. GISMO
and NIKA, the two prototype continuum arrays now
produce unique science and pave the technological
way to a future facility continuum instrument.
The PdBI Interferometer has produced a wide range
of top-level science results ranging from very exiting
investigations on galactic low mass star formation
to observations in the distant universe with deep
impact on the understanding of how galaxies form.
The year 2012 has also seen ALMA producing
its first science results. The high success rate of
proposals from members of the IRAM community
clearly shows the advantage that our users have. A
highly competent support through the IRAM ARC
has been put into place and is receiving excellent
user feedback. Towards the end of 2012, IRAM
has successfully finished its production of ALMA
B 7 cartridges. The first round of regular ALMA
observations shows that this band with its excellent
performance and reliability will play a central role in
the operation of ALMA.
Undeniably the economic situation in Europe has
degraded, and IRAM is forced to adapt with very
tight budget constraints. It is remarkable that IRAM
can pursue in such difficult times ambitious projects
like NOEMA, a further proof of the outstanding
support from the partner organizations CNRS, MPG
and IGN. Although numerous investments on new
instruments must be postponed due to the budget
situation, basic technical developments can be
continued (also with the help of European funding
FP7 Radionet), a fact which will allow IRAM to
maintain its know-how and leading position in mmwave instrumentation.
At the time when this report is edited, another
important change at IRAM has taken place. After
more than 8 years of duty as the IRAM director, Pierre
Cox has started his new position as the director of
ALMA in Santiago, Chile. I thank Pierre Cox in the
name of the IRAM staff and the IRAM partners for
his collaboration, his continuous effort, and his
involvement in numerous and sometimes difficult
undertakings. Together with Frederic Gueth, the new
deputy director, and the IRAM staff, we will continue
with all our determination to keep IRAM up and
ready for the many exciting things to come in the
future of millimeter astronomy.
Karl-Friedrich Schuster
Director
5
6
Institut de Radioastronomie Millimétrique
Highlights of research with
the IRAM telescopes in 2012
LARGE FLUORINE RESERVOIRS IN THE HORSEHEAD NEBULA
observed but of critical importance for the chemical
synthesis of new molecules.
Various efforts have been directed in the last years
at astronomical line surveys, theoretical chemistry
calculations of gas phase reaction rates and
laboratory measurements. In an effort to provide
observational constraints, Viviana Guzman (IRAM)
and collaborators used the IRAM 30m telescope to
conduct a line survey targeted at two positions in
the Horsehead nebula: the warm UV-illuminated gas
(PDR) and the cold UV-shielded gas (dense core).
Embedded within a forest of molecular lines from
many species, Guzman et al clearly identified
the weak chemical signature of CF+, the fluoromethylidynium ion. This molecule is not only
of considerable interest to assess the chemical
abundances and spatial distribution of HF and C+
in the environment of PDRs but also to evaluate its
reliability as a possible proxy for C+ in the study of
galactic chemical factories.
DCO+, HCO (left) and CF+
(right) integrated line
intensity maps of the
Horsehead Edge. The vertical
line (red) identifies the edge
of the photo-dissociation
region (PDR); the crosses
identify the center of the
PDR (green) and of the dense
adjacent molecular core
(blue).
Work by Guzman et al. 2012,
A&A, 543, L1
Understanding the chemistry of photo-dissociationdominated regions (PDRs) is undoubtedly one of the
key research areas in observational astrophysics. The
goals are to measure reliable molecular abundances
in PDRs, compare them to state of the art of
astrochemical models to understand the formation
and destruction mechanism at work, and dare to
predict the existence of molecules, too rare to be
Guzman et al. combined the Meudon (Le Bourlot et
al. 2012) photochemical model with the observed
30m telescope data to predict the abundances
of CF+, C+ and HF in the PDR at the edge of the
Horsehead Nebula, and concluded on a CF+
abundance of ~10-5 relative to C+, and on a 4–8%
amount of fluorine directly locked within CF+.
Chemical models predict that CF+ and C+ coexist; this
strongly suggests that CF+ is a good proxy for C+ and
is tracing the outer C+ layer of the PDR.
Annual report 2012
7
A PETROLEUM REFINERY IN THE MILKY WAY
The study of complex molecules in space is crucial
for understanding the physical and chemical
processes in the interstellar medium (ISM). As ISM
regions are often characterized by a high diversity
of molecular species, identifying the spectral
signature and diagnosing their chemical properties
is becoming a challenge in itself. The majority
of interstellar molecules have been detected at
millimeter wavelengths, as molecules with small
lines towards the PDR, and they tentatively assigned
them to the spectral signature of l-C3H+. Laboratory
measurements are needed now to refine the
spectroscopic characterization of the newly detected
molecule. This molecule, the so-called propynylidyne
cation, is part of the hydrocarbon family, which
composes one of the major energy sources on Earth,
petroleum and natural gas. From the observations,
the authors infer a column density of 5.1011 cm-2 and
moments of inertia are the most abundant and their
rotational transitions are observable in the millimeter
range. As of today, extensive spectral line surveying
made it possible to identify the spectral signatures of
about 200 molecules in the ISM.
a relative abundance of 10 for l-C3H at the edge
of the Horsehead PDR, and in good agreement with
the predictions of a photochemical model of the
PDR. In contrast, the same model cannot account for
the measured amounts of other small hydrocarbons
like C2H, C3H, C3H2, and C4H. Pety and collaborators
suggest that these small hydrocarbons result from
the fragmentation of PAHs by erosion through UV
radiation. The mechanism is likely to be particularly
efficient in regions like the Horsehead Nebula where
the interstellar gas is directly exposed to the light of
a nearby massive star.
Inspired by the success of the EMIR receivers and
of the Fourier Transform Spectrometer (FTS) at
the IRAM 30m telescope, a team led by Jérôme
Pety (IRAM/ LERMA) embarked on the Horsehead
WHISPER survey. WHISPER is major effort aiming at
characterizing the physical and chemical conditions
in two areas of the Horsehead nebula: the photodissociation region (PDR) at the edge of the nebula
and a nearby colder condensation. On analyzing
the results generated by their complete spectral
line surveys over three bands of the EMIR receivers,
the researchers discovered a set of unidentified
-10
+
The survey enabled the detection of about 30
molecular species. Among these small hydrocarbons
like C2H, l-C3H, c-C3H, l-C3H2, c-C3H2, and C4H were
found.
IRAM 30m EMIR/FTS spectra
profiles and Gaussian fits
(green) of l-C3H+, C2H, l-C3H,
c-C3H, l-C3H2, c-C3H2, and C4H
towards the Horsehead PDR.
Work by Pety et al. 2012, A&A,
548, A68
8
FIRST IDENTIFICATION OF A PRE-BROWN DWARF
Brown dwarfs lie
between planets and
stars in terms of mass
and composition. They
are too light to undergo
hydrogen fusion but too
massive to be called a
planet. Their predicted
masses range from
about 0.014 to 0.075
M⊙, although the mass
boundary with planets is
subject to debate.
(top) N2H (1-0) image of Oph
B-11 obtained with the IRAM
interferometer. The filled
triangle shows the position of
the 3.2 mm continuum peak.
(bottom) N2H+(1-0) spectrum
resulting from combined
IRAM interferometer and 30m
telescope observations.
Work by André et al. 2012,
Science, 337, 69
+
Today, two competing
formation scenarios
exist for brown dwarfs:
1) formation as a byproduct of the process
of disk fragmentation
and/or ejection, 2)
formation from the
direct collapse of a selfgravitating condensation
of gas and dust, a socalled pre-stellar core.
In the second formation
scenario, a large number of ultra-low mass cores are
predicted to be dense enough to be gravitationally
unstable to collapse. However, the existence of such
pre-brown dwarf cores had never been confirmed
observationally.
To demonstrate the existence of pre-brown dwarfs
and provide support to models where brown-dwarfs
form like solar-mass stars, Philippe André (CEA-IRFU)
and collaborators pointed the IRAM interferometer
on Oph B-11, a starless core in the cluster-forming
region L1688.
They obtained a robust detection of the source in
both the continuum at 3.2 mm and the N2H+(1-0)
line. They fitted the visibilities with a Bonnor-Ebert
core model and yielded a best-fit size of 1.0±1.8” for
the outer angular radius, and a best-fit core radius
of 140 AU. The continuum was detected at the
0.4mJy level and found consistent with emission
originating from a region of cold gas and dust (≤10K)
and of enhanced H2 column density (≥∙71022 cm-2).
From this, the gas and dust mass of Oph B-11 was
estimated to 0.02-0.03 M⊙. The linewidth of the
N2H+(1–0) transition was found to be extremely
narrow (0.2 km/s) indicating that the velocity
dispersion of the gas within the core is nearly
thermal and comparable to the isothermal speed of
sound.
As no other stars or proto-stars were found to
form close to Oph B-11, André and collaborators
concluded from these observations that pre-brown
dwarfs do exist and that brown dwarfs may form
from the direct collapse of low-mass pre-stellar
cores.
PREBIOTIC CHEMISTRY IN PROTOPLANETARY SYSTEMS
Protoplanetary disks are rotating disks of gas and
dust surrounding young stars. On their route to
(top) low-resolution spectrum
of HC3N and H2CO towards
LkCa15 in the 3.5” beam of
the IRAM interferometer,
(bottom) high-resolution
image (0.5”) of the 1.3mm
thermal dust emission from
the circumstellar disk of
LkCa15.
Work by Chapillon et al. 2012,
ApJ, 756, 58
forming stars, they appear to dissipate remnant gas
and dust and lead to the formation of planetary
systems. As these objects
are believed to be the
birthplace of planets,
detailed studies of their
structure, composition
and properties are
expected to shed light on
the origin of planets.
Using the IRAM 30m
and Plateau de Bure
interferometer (PdBI),
a team led by Edwige
Chapillon (Academia
Sinica) reported
the detection of
cyanoacetylene (HC3N)
Annual report 2012
in the disks of two solar-like objects, the low-mass
stars LkCa15 (PdBI, IRAM 30m) and GO-Tau (IRAM
30m), and of the more massive star MWC480 (IRAM
30m). LkCa15 is considered to be peculiar, as it
shows a disk cavity, a telling sign of the formation of
a planetary system. The authors presume a Jupiterlike planet, whose presence is inferred from infrared
excess emission, carved it out.
HC3N is the heaviest and most complex molecule
ever detected in a protoplanetary disk so far. It is
the simplest cyanopolyyne, and presumably, also
one of the key elementary bricks in the formation of
complex organic molecules and in the emergence of
life. According to current models of disk chemistry,
HC3N is mainly formed through grain surface
reactions in the colder regions (≤15 K) near the disk
mid-plane. Contrary to HC3N, simple molecules like
9
CO and H2O are frozen onto the grains’ ice mantle in
the inner disk layers. These molecules can undergo
a variety of reactions on an ice grain mantle to form
more complex species. The newly formed molecules
can then be released into the gas-phase by thermal
evaporation or via induced desorption by ultraviolet
radiation and cosmic rays. As the observed column
densities of HC3N (~1012 cm-2) are found to be
lower by two orders of magnitude than predicted,
Chapillon and coauthors suggest that the mid-plane
molecular chemistry is sensitive to the UV radiation
field.
The discovery of HC3N in these three planetary
formation regions is an important first step towards
understanding the emergence of prebiotic
molecules on Earth and exoplanetary systems.
THE AFTERMATH OF TWO EXPLOSIVE MASS-LOSS EVENTS IN M2–9
Understanding the appearance and shaping of
bipolar winds in the transition of stars from the late
asymptotic giant branch (AGB) to the planetary
nebula (PN) phase is one of the most challenging
issues in stellar evolution. Bipolar winds are not
only critical to unraveling the AGB to PN evolution
timescales but also to characterize how PN
properties are shaped by wind interactions. One
mechanism invoked to account for the generation
of bipolar winds is the presence of an orbiting
binary star system at the nebula’s center. While the
direct detection of a binary companion is currently
a challenge, its presence can be inferred indirectly
through its dynamical influence on the surrounding
circumstellar material. Currently, the best way to
measure its dynamical imprint in regions, which
normally are hidden to optical telescopes, is with
sensitive interferometric observations in the
millimeter waveband.
M 2–9, which is one of the few established examples
of a bipolar planetary nebula in the making, is one of
the most promising candidates to gain initial insights
into the orbital geometry of the presumptive binary
star system. IRAM Plateau de Bure interferometer
observations of M 2–9 by Arancha Castro-Carrizo
(IRAM) and collaborators have recently unveiled two
ring-shaped structures in the waist of the nebula,
both fitting remarkably well the basal point of
departure of the optical lobes.
The rings were ejected during two short episodes (of
≤40 yr), about 1400 yr and 900 yr ago. The centers of
the two rings were found offset by 220 AU and their
systemic velocities by 0.6 km/s. According to the
authors these findings provide sound evidence for
the presence of a binary star system in M 2–9.
The two rings were very probably ejected by one
of the stars, in a very late AGB or very early postAGB phase. Different positions in the stars orbital
motion explain the measured position and velocity
offsets between the rings. At the
same time, two independent
mass-loss events seem to have
corseted the expanding nebula
into the classic hourglass shape
typical of many PN. By analyzing
the kinematics of the equatorial
rings and assuming a mass of
0.5 – 2 M⊙ for the primary star,
Castro-Carrizo and collaborators
estimated the mass of the
secondary to ~0.2 M⊙ and its
orbital speed to ~1 km/s. They
also suggested the binary
system is composed of a red
giant and a dwarf, separated by
~20 AU, a distance considered
too large for the stars to have
undergone a common envelope
phase, or for being interacting
members of a symbiotic system.
Velocity integrated 12CO
J=2-1 line emission towards
M 2–9 (inset) superposed on
the HST/WFPC 2 image (light
blue).
Work by Castro-Carrizo et al.
2012, A&A, 545, A1
10
Surface mass densities of
molecular (left panel) and
atomic hydrogen (middle
panel), and total gas (right
panel) as a function of the FIR
surface brightness at 250 μm.
Different symbols distinguish
non-deficient (red circles),
slightly HI-deficient (black
triangles), and HI-deficient
galaxies (blue stars).
Work by Pappalardo et al. 2012,
A&A, 545, A75
ENVIRONMENTAL EFFECTS ON VIRGO CLUSTER GALAXIES
The stellar and gas distributions in a cluster
galaxy can be drastically modified through
environmental effects. While a spiral galaxy can
lose a considerable fraction of its neutral gas (HI)
through tidal interaction with neighbor galaxies
and/or ram-pressure stripping, molecular gas is
more bound to the galaxy potential and therefore
less prone to removal via stripping. Indeed, in Virgo,
a young, close (D~17 Mpc) and still dynamically
active cluster, the environment effects are clearly
seen for the atomic gas but are less evident for the
molecular gas phase. Also while the global dust-tostellar mass ratio is found to decrease as a function
of HI deficiency, the dust-to-total-gas ratio is found
to increases.
To develop a better understanding of the complex
interplay between the different constituents of the
ISM at various galactic distances and environmental
effects, Ciro Pappalardo (INAF/Arcetri) started an
international collaboration. The team observed
a sample of 7 Virgo galaxies in the 12CO (1-0) and
(2-1) transitions with the IRAM 30m telescope
and combined the results with literature data.
It estimated the integrated mass of molecular
hydrogen for the galaxies observed in the CO lines
and inferred molecular-to-total gas mass fractions
between 0.04 and 0.65, and integrated dust-to-gas
ratio ranges between 0.011 and 0.004.
According to Pappalardo and collaborators, both
the molecular gas and the dust distributions show
steeper radial profiles for HI-deficient galaxies and
the average dust-to-gas ratio for these galaxies
increases or stays radially constant. On scales of ~3
kpc, they find a strong correlation between the
molecular gas and the 250 μm surface brightness.
The correlation, is found tighter than average for
non-deficient galaxies, and becomes linear if the
total gas surface mass density is considered. The
inclusion of atomic hydrogen does not improve the
statistical significance of the correlation.
THE METALLICITY DEPENDENCE OF THE CO/H2 CONVERSION FACTOR
IN Z>1 SFGS
H2 is the primary but elusive component of
the reservoirs of cold, dense gas that fuel star
formation in galaxies. Estimates of gas masses
and surface densities are therefore often derived
from observations of CO using the galactic CO/
H2 conversion factor. While the canonical value of
αCO=4.36 is adopted for a Milky Way like ISM, surface
densities derived from CO are likely to be biased if
the same conversion factor is used for galaxies with
a metallicity (or dust-to-gas ratio) very different from
that of the Milky Way.
To explore the metallicity dependence and evolution
over cosmic time of the CO/H2 conversion factor in
z>1 “main-sequence” star-forming galaxies (SFG),
Reinhard Genzel (MPE) and collaborators used
a first systematic sample of CO measurements
from the IRAM interferometer, and metallicities
derived from [NII]/Hα estimates and stellar-massmetallicity relations at the SFG redshifts. The survey
encompasses a sample of 37 SFGs, including 21
galaxies from two IRAM Large Programs.
According to the study, the molecular gas depletion
rate inferred from the ratio of star formation rate
(SFR) to CO luminosity is ~1 Gyr−1 for near-solar
metallicity galaxies with stellar masses above
MS~1011 M⊙. In this regime, the depletion rate does
not vary more than a factor of two to three as a
function of molecular gas surface density or redshift
between z~0 and 2. Below MS the depletion rate
increases rapidly with decreasing metallicity.
Annual report 2012
CO-based Molecular gas
depletion rate as a function
of molecular gas surface
density. The open gray circles
are non-mergers, near-mainsequence, and moderately
high-mass SFGs at z~0. Blue
circles, black triangles, and
red squares denote z>1 SFGs
from the IRAM LP program
and other data in three
metallicity ranges. In this form
of the KS-relation, constant
molecular depletion times or
rates are horizontal lines.
Work by Genzel et al. 2012,
ApJ 746, 69
The researchers argue that this trend is not caused
by starburst events, by changes in the physical
parameters of the molecular clouds, or by the impact
of the fundamental-metallicity–SFR–stellar mass
relation. A more probable explanation is that the
conversion factor is metallicity dependent and that
star formation can occur in “CO-dark” gas.
The trend is also expected theoretically from the
effect of enhanced photodissociation of CO by
ultraviolet radiation at low metallicity. From the
available z~0 and z~1–3 samples they constrain the
slope of the log (αCO)–log (metallicity) relation to
range between –1 and −2, fairly insensitive to the
assumed slope of the gas–SFR relation. Because of
the lower metallicities near the peak of the galaxy
formation activity at z~1–2 compared to z~0, they
11
suggest that molecular gas masses estimated from
CO luminosities have to be substantially corrected
upwards (by factors of 2 to 10) for galaxies below MS.
NITROGEN EMITTERS AT HIGH REDSHIFT
Forbidden atomic fine-structure transitions are
important cooling lines of the interstellar medium
(ISM). They provide effective cooling in cold regions
where allowed atomic transitions cannot be excited,
and thus are critical diagnostic tools to study the
star-forming ISM. One of the most important cooling
line is the forbidden 2P3/2–2P1/2 fine-structure line of
ionized carbon at 158 μm, which alone accounts
for 0.1%–1% of the total continuum far-infrared
(FIR) luminosity in local, star forming galaxies. Other
main cooling atomic transitions are provided by the
FIR lines of [OI], O[III] and [NII]. Due to its ionization
energy, the fine-structure line of [NII] 205 μm is
generally an excellent tracer of the ionized medium
around star-forming regions.
Last year’s annual report showed the results of
the highest redshift detection (z = 5.24) of [NII] at
205 μm. New observations have now been made
by a team led by Roberto Decarli (MPIA) that
yielded secure fine-structure line detections in
two millimeter-bright and strongly lensed objects:
APM08279+5255 (z=3.911) and MM18423+5938
(z=3.930). Both objects were observed with the
IRAM Plateau de Bure Interferometer by using the
capabilities of the band 4 receivers (275 – 373 GHz)..
The data revealed intrinsic [NII] line luminosity of
~1.8 109 L⊙/μ for APM 08279+5255 and ~2.8 109 L⊙/μ
for MM 18423+ 5938.
The high-resolution map of the [NII] and 1.0 mm
continuum emission in MM 18423+ 5938 clearly
resolves an Einstein ring in this source and reveals a
velocity gradient in the dynamics of the ionized gas.
The authors measure a [NII]/FIR luminosity ratio of
~9.0 10-6 on APM 08279+5255 and of ~5.8 10-6 in
MM 18423+5938, which they found in agreement
with the decrease at high FIR luminosities observed
in local galaxies.
High-resolution (0.6”x0.5”)
map of the line-free
continuum emission in MM
18423+5938 with contours
in steps of 4σ (top left);
continuum subtracted map
of the [NII] emission with
contours in steps of 2σ (top
right); color-composite
image of red and blue [NII]
line emission wings with
overlaid the contours of the
continuum map (bottom left).
Bottom right: comparison
of the [NII] line map (white
contours), the continuum
emission (black contours),
and the 12CO(2–1) map
published by Lestrade et al.
(2011) (color scale). Work by
Decarli et al. 2012, ApJ, 752, 2
12
Spectra of the H2O (left,
(211−202) or (202−111)) and 12CO
(right, 3−2, 4−3, 5−4 or 7−6)
emission lines observed at the
IRAM interferometer towards
six lensed H-ATLAS galaxies
(top), lensing corrected H2O
to infrared luminosity ratio for
a sample of ultra-luminous
infrared galaxies at low and
high redshift (bottom).
Work by Omont et al. 2013,
A&A, 551, 115
LUMINOUS WATER VAPOR EMISSION AT HIGH-Z
Water is a molecule of key importance in
astrophysical environments. In cold molecular
clouds, water is in the form of icy mantles on dust
grains but in warm and dense (≥100K, ≥105 cm−3)
clouds, such as in starbursting galaxies or galaxies
with a luminous active galactic nucleus, water
can evaporate from the dust grains when the
grain temperature becomes sufﬁciently high or
via photodesorption by exposure to high-energy
radiation. Water is then one of the most abundant
oxygen-bearing molecules after CO and an
important coolant of the warm and dense gas, and
as such it must play an important role in the process
of star formation.
To evaluate the potential of water as a key diagnostic
tool to probe both the extreme physical conditions
and the infrared radiation in the warm dense
environments of high-redshift starbursting galaxies,
Alain Omont (IAP) and coauthors observed a sample
of six, strongly lensed Herschel H-ATLAS galaxies with
the IRAM interferometer.
The team was able to report the detection of water
vapor line emission in the warm and dense core
of all six galaxies with redshifts in the range from
1.57 to 4.24. The derived H2O luminosities corrected
for lensing magnification show a strong ~LIR1.2
dependence on the galaxies’ infrared luminosity.
Though the measured slope of the LH2O/LIR relation is
affected by uncertainties in the lensing factors, the
relation suggests that infrared pumping is playing
a key role in the excitation of the H2O lines. Water
emission is therefore expected to become very
strong in the most luminous (LIR>1013L⊙) galaxies.
Omont et al detections of the water vapor emission
lines in these six luminous galaxies demonstrate
that the millimeter/submillimeter transitions of
water vapor provide a powerful tool to probe the
warm, dense and dusty molecular environments
in luminous infrared galaxies at high redshift.
Observations in other water lines and molecular
species are planned with ALMA and NOEMA and
will possibly help to further constrain the excitation
conditions and the water abundances in these
regions.
Annual report 2012
13
MYSTERY OF GALAXY HDF850.1 FINALLY SOLVED
The region in the sky where HDF850.1 is located
affords an almost unparalleled view into the deepest
reaches of space. Known as the Hubble Deep Field
(HDF), it was first studied extensively in visible light
with the HST. Yet these observations only reveal
part of the cosmic picture, and astronomers were
quick to follow-up the Hubble observations with
other telescopes operating at longer wavelengths.
In the late 1990s, astronomers surveyed the region
using the SCUBA/JCMT. The researchers were taken
by surprise when they realized that HDF850.1 was
the brightest submillimeter source in the field by
far, a galaxy that was evidently forming as many
stars as all the other galaxies in the HDF combined,
presumably one of the most productive star-forming
galaxies in the observable universe – and which was
completely invisible in the observations of the HST.
An international team of astronomers led by Fabian
Walter (MPIA) finally managed to determine the
distance of HDF850.1 with the IRAM interferometer.
Taking advantage of recent instrumental upgrades
they were able to identify the (6-5) and (5-4) lines of
12
CO and to detect the redshifted 2P3/2–2P1/2 transition
of [CII]. By combining these results with a 12CO (2-1)
detection by the VLA, Walter and collaborators
determined the redshift of HDF850.1 to 5.183
corresponding to a lookback time of ~12.5 Gyr. They
also put first constraints on the physical properties
of the host galaxy: the [CII] line luminosity was
estimated to ~1.1 1010 L⊙, the FIR luminosity to ~6.5
1012 L⊙, the total dust mass in the host galaxy to ~2.8
108 M⊙, and the global star-formation rate to ~850
M⊙/yr. Based on the size of the [CII] emission region,
the authors derived a star formation rate density
of ~35 M⊙/yr/kpc2. The linewidth was estimated
to 400 km/s (FWHM) and found narrower than in
submillimeter-selected galaxies.
Once the redshift was known, the astronomers were
able to put the galaxy into context. Using additional
data from published and unpublished surveys, they
were able to show that the galaxy is part of a group
of a dozen other galaxies, spread over six million
light-years, all formed within the first billion years of
cosmic history. At this redshift, only one other galaxy
group like this is known so far (Riechers et al. 2010).
EXTREME QUASAR FEEDBACK IN THE EARLY UNIVERSE
Most theoretical models invoke quasar driven
outflows to quench star formation in massive
galaxies, and this feedback mechanism is required
to account for the population of old and passive
galaxies observed in the local universe. The discovery
of massive, old and passive galaxies at z~2, implies
that such quasar feedback onto the host galaxy
must have been at work very early on, close to the
reionization epoch. Evidence for such feedback has
been found only recently in quasar hosts through
the discovery of massive outflows: Herschel Space
Telescope spectra have revealed prominent [CII]
emission associated with molecular outflows of
nearby quasars but quasar-driven outflows have
been uncovered also at high redshift.
In a concerted effort to advance understanding on
quasar negative feedback, a team led by Roberto
Maiolino (University of Cambridge) used the IRAM
interferometer to observe SDSSJ1148+5251 at
z=6.42 in the [CII] 2P3/2–2P1/2 line, and discovered
an exceptional outflow in the host galaxy of this
remarkable quasar. The outflow velocity (~1300
km/s), luminosity (~7.3 109 L⊙) and kinetic power
(>1.9 1045 erg/s) are clearly in favor of quasar
radiation pressure as the main driving mechanism.
Based on the interferometer data, the authors also
estimated a lower limit to the total outflow rate
(~3500 M⊙/yr), which they found higher than the
star formation rate in the quasar host (~3000 M⊙/yr),
and the extent of the outflow to smaller than 16 kpc.
Spectra of the redshifted [CII]
at 158 um and of the (6-5),
(5-4) and (2-1) transitions of
12
CO, with the underlying
continuum. The (2-1)
transition was marginally
detected at the VLA.
Work by Walter et al. 2012,
Nature, 486, 233
14
IRAM interferometer
continuum subtracted
spectrum of the redshifted
[CII] 2P3/2–2P1/2 line towards
J1148+5251.
Work by Maiolino et al. 2012,
MNRAS, 425, L66
From all this, Maiolino and collaborators conclude
that SDSSJ1148+5251’s outflow is a cornucopia of
superlatives: it is the most distant, most massive and
possibly also the largest outflow ever detected.
The authors conclude that at the inferred massloss rate, the host galaxy’s gas reservoir would be
swept out in less than 6 106 yr and star formation
in the galaxy host would rapidly be damped down.
Their findings therefore support models ascribing
the capability of cleaning entire galaxies, out to
large radii, to quasar-driven outflows. According to
Maiolino and collaborators, such a fast and efficient
quenching mechanism, already at work at z>6, is
what is required by models to explain the properties
of massive, old and passive galaxies observed in the
local Universe and at z~2.
Annual report 2012
15
The 30-meter telescope
OVERVIEW
Within the wide range of technical work one
particular focus of 2012 was to further improve
the integration of the newly installed Fast Fourier
Transform Spectrometers (FTS) exploiting the
large bandwidths provided by the eight-mixers
receiver EMIR. The combination of FTS with EMIR is
increasingly used for frequency surveys studying
the complex chemistry of a variety of sources, from
comets, pre-stellar cores, and Galactic star-forming
regions, to the nuclei of nearby galaxies, and finally
also for unbiased searches of CO and other lines
to obtain accurate redshifts of distant galaxies. The
study of the prototypical ultra-compact HII region
MonR2 is just one example of such work, which also
shows the power of combining frequency-surveys
with spatial maps of the observed objects.
Frequency survey of the
ultra-compact HII region
Mon R 2 using EMIR and the
FFT-Spectrometers (Trevino et
al. in prep.)
16
Galactic Center region
observed with GISMO/30m
at 2mm (green) in April 2012
with LABOCA/APEX at 850um
(blue), and with the VLA at
20cm (red). (Morris, Staguhn
et al. in prep.)
Another focus of work in 2012 has been to continue
the integration and testing of the two new
prototype continuum cameras GISMO and NIKA.
In April 2012, GISMO was offered for the first time
to the community during two weeks of pooled
observations. One science high-light of this run has
been the map of the Galactic Center region obtained
during only 6 hours of observing time showing
the importance of the 2mm emission tracing not
only the extended molecular clouds, but also the
thermal and non-thermal radio continuum filaments.
Also, the NIKA camera with its two arrays of Kinetic
Inductance Detectors (KID) working simultaneously
at 2 and 1mm, made strong progress as discussed
further below. One example of the test run in
November 2012, is the successful mapping of the
Sunyaev Zel’dovich (SZ) effect towards an X-ray
cluster of galaxies improving on observations done
about 10 years ago with the Diabolo-camera at the
30m telescope, and paving the way for SZ-studies of
the hundreds of clusters found by Planck, ACT, and
STP with the future, new, large field-of-view dualband camera NIKA-2.
ASTRONOMICAL PROJECTS
During the year 2012, a total of 208 projects were
scheduled at the 30m telescope, including 4 large
programs. A fraction of 26% of these projects was
scheduled in the heterodyne and continuum
observing pools. A total of 149 astronomers visited
the telescope in 2012, 42 of which came to support
the observing pools. About 20% of the scheduling
units, mainly the shorter ones of typically less than 10
hours, were observed remotely. From the proposals
eligible for RadioNet support, 32 were scheduled at
the telescope, and 7 European astronomers were
granted travel support.
The vast majority of the scheduled projects used
EMIR (87%). The remainder is made up by HERA (5%)
and the 2mm bolometer camera GISMO (8%). The
total observing time was split by about half between
Galactic and extragalactic projects.
TIME DISTRIBUTION
Usage statistics of all 4 EMIR
bands in 2012
The IRAM 30m telescope operates 365 days per year,
at 24 hours per day. The figure “Time distribution
in 2012” shows that more than 70% of the total
time was spent for astronomical observations, a
number which has been very constant over the
past few years. About 8% of the total time was used
for maintenance and tests. Slightly more than one
fifth of the total time were lost for astronomical
observations due to adverse meteorological
conditions, and less than 0.5% of the total time were
lost due to technical problems, about half due to
problems in the computer / network area (see the
section on Computers).
Annual report 2012
17
Monthly time distribution of
observing time (U.Observ.),
technical projects (U.T.T.),
maintenance (U.Mainten.),
time lost due to high wind
speeds (S.Wind), or other
adverse meteorological
conditions (S.Meteo), or
technical problems (S.Techn.).
TELESCOPE OPERATION
In September 2012, the last two new gearboxes were
installed at the 30m telescope. With this intervention
the replacement of all six gearboxes, which started
in 2010, has been successfully finished. The new
gearboxes were built by the Germany company
Desch which will also provide the gearboxes for the
new antennas of NOEMA. In a series of detailed tests,
we confirmed that their characteristic properties
(stiffness, resonance frequencies, hysteresis, rolling
friction, brake behaviour, vibrations) have reached or
exceeded the specifications.
After more than 30 years of operation, several of the
antenna surface panels have started to loose their
top layer of paint. Images taken with an infrared
camera show somewhat increased temperatures of
the blackened panels when pointing near the sun.
An investigation has started on how to possibly
repaint the primary mirror. For this, Vertex and MT
Mechatronics have provided samples of paint of
different properties, put on small aluminium panels.
Their mm-wavelength properties are now being
characterized by the frontend group in Grenoble.
In parallel, we have started to prepare again for
holographic measurements of the primary surface
using the 39GHz beacon of AlphaSat, a new satellite
which is scheduled to be launched in June 2013 (see
the section on Frontends).
In the course of 2012, several measures were taken
to further improve safety at the 30m. On 20-June,
we have simulated a human emergency inside
the motors room of the 30m telescope. In this
simulation, which was the first of its kind at the 30m,
the local 061 service for medical emergencies, the
service 112 for general emergencies, and the Guardia
Civil worked tightly together with the IRAM staff at
the telescope to “rescue” one of the staff members
via helicopter to Granada. A video live-link to the
061 emergency support service has been prepared
to receive medical advice if needed. On 14-June, the
Granada fire brigade gave a general fire prevention
training course, which we are conducting every 2
years at the observatory. On 15-October, 10 staff
members participated at a specific training course
of the Granada fire brigade on using the oxygen
breathing equipment. We plan to repeat this course
at regular intervals.
FRONTENDS AT THE 30M TELESCOPE
After more than three years of continuous operation
the EMIR receiver has proven to be the core of the
frontend section at the 30m telescope. The receiver
is being upgraded continuously, both by increasing
its RF and IF bandwidths and by expanding the
capabilities of the associated equipment. Examples
of this are the modification of the IF switch box
in order to allow new combinations of the 2mm
band and the installation of a remotely controllable
heating element for removal of quantum flux
trapping on the E 230 band.
Shortly after the installation of the new 1.3 and 0.8
mm mixers, in fall 2011, a problem was detected on
the E 230 band. Spurious lines were contaminating
many of the frequencies on both sidebands and
18
poor weather conditions and from problems with
the new taumeter. During the November run, we
used the old taumeter for atmospheric calibration.
NIKA 2mm map of the Sunyev
Zel’dovich decrement toward
the X-ray cluster RXJ1347.51145 taken in November 2012.
(Desert et al. in prep.)
polarizations. An intensive search for the cause, lead
to the identification of internal oscillations in the
mixer-cold IF amplifier assembly. The oscillations
were eliminated in spring 2012 by modifying the
bias and LO power level settings with none or little
degradation in receiver temperatures.
The Goddard-IRAM 2mm 30m observatory (GISMO)
camera has been offered to the astronomical
community for the first time during two runs in
April and November 2012, over a total of 4 weeks.
This prototype camera uses super-conducting
transition edge sensors (TES) and SQUIDs for
readout. In preparation for the first open run of
pooled observations, a new optics, which had been
designed at IRAM/Grenoble, was installed using
less mirrors together with a new extra cold baffle
to improve the sensitivity by stray-light mitigation.
GISMO was moved to a new place in the receiver
cabin allowing observations at low elevations, and
allowing a dual installation of GISMO together
with NIKA. During the GISMO runs, IRAM receiver
engineers learned handling of the cryostat. A
long-standing leak problem on the GISMO cryostat
was found and corrected by replacing the cryostat
window. The improved vacuum reduced the
cryogenic liquids consumption to half the previous
rate. At present, GISMO needs to be recycled once
per day. Median GISMO sensitivities have reached
~13mJy ∙s1/2, dominated by sky noise, with about
100 healthy pixels of the 8x16 array (1.8 arcmin x
3.7 arcmin). Data are now routinely processed by an
automatic data pipeline using CRUSH (A. Kovàcs).
The pipeline is producing preliminary results and
puts them online. The relative flux stability has been
better than 10% during the April run, and somewhat
worse for the November run which suffered from
Tests with the prototype New IRAM KIDs Array
(NIKA) continued during two runs in June and
November 2012. NIKA is a dual-band prototype
camera (P.I.: A.Benoit, Neel Institute/Grenoble) with
two kinetic inductance detector (KID) arrays working
at 2 and 1mm, using a 45deg dichroic mirror to
split the wavebands. NIKA uses a 4K cryocooler
and a closed-cycle dilution to achieve its 150mK
working temperature. The data acquisition rate is
22Hz synchronously over each array. Fits files are
provided that contain raw data and the central
resonance frequency of each KID which is assumed
to be proportional to the incoming millimeter
power. The run in November 2012, showed that
the best pixels reach sensitivities with 18mJy.
sqrt(sec) at 2mm and 24mJy.sqrt(sec) at 1mm. The
test runs allowed to progress in the development
of the arrays, electronics, data readout, and data
processing, while at the same time identifying a
number of issues on which we will improve, in
preparation of a commissioning run of NIKA in 2013,
and in preparation also for the large, new continuum
camera at the 30m telescope, NIKA-2.
The HEMT 3mm receiver was modified in Grenoble
to include new metamorphic HEMT amplifiers
designed within the AMSTAR+ project. The receiver
was installed and successfully tested at the 30m
telescope during the summer season. An optics with
extended frequency range optics (75-116GHz) has
been designed and is planned to replace the existing
one in the future.
Work started on the modification to the holography
receiver and the data acquisition system in
preparation for measurements of the antenna
surface. The acquisition part of the modification
consisted in the migration from an obsolete
Windows based PC operating system to a Linux
based system together with subsequent software
modifications. In addition, the frequency of the
receivers had to be adapted to 39.4GHz.
Annual report 2012
VLBI
In autumn 2012, the hydrogen maser for VLBI,
EFOS-10, has been sent to T4Science in Neuchatel/
Switzerland for repair with the aim to solve sporadic
out-of-locks. Another maser, EFOS-21, has been
rented by the MPIfR/Bonn and installed at the
telescope to carry out observations during the
2012/13 winter period.
The European model of the Digital Base Band
Converter (DBBC) VLBI backsend was installed with
help from MPIfR engineers. It replaces the analog
rack with Mark4 recorder. The new DBBC works with
a new series of disk recorders Mark5B and Mark5C.
With this backend a peak data rate of up to 8Gbits/s
might be expected.
BACKENDS AT THE 30M TELESCOPE
The 24 units of Fast Fourier Transform Spectrometers
(FTS), which were installed in 2011, are working
very well with no failures. Some observations
using large bandwidth do however suffer from
baseline “platforming” between individual FTS units.
An investigation in the labs of the MPIfR in Bonn
confirmed that small temperature drifts of the 8bitADCs cause small total-power drifts of the individual
units against each other. This situation cannot be
easily improved. The FTS are therefore of limited use
as continuum detectors of faint sources.
To prepare for a future upgrade to 64GHz bandwidth
using FTS/EMIR, and for the 3mm 5x5 dual-channel
multi-beam 3mm receiver, we have studied jointly
with the Grenoble backend group the option to
use an optical microwave link to transport the
intermediate frequencies (IF) to the backends. At
present, they are transported via thick 4GHz coaxial
cables through the cable spiral of the telescope into
the backend room. The optical fiber was carefully
evaluated through a combination of on-sky and
laboratory measurements. These tests showed
degraded baselines and insufficient dynamic range
taking into account the large power level changes
during calibration and the bandpass ripple of the
receivers. We are therefore considering alternative
solutions to the IF transport, as e.g. thin 3 / 8” coaxial
cables.
The design of a barycentric reference progressed
significantly in a joint effort by the backend groups
in Granada and Grenoble. The goal is to eliminate
the need for resampling of spectra taken with
large bandwidths and high spectral resolutions.
This software solution currently degrades the
instrumental resolution when simultaneously
observing with the same receiver widely separated
lines (up to 24GHz with EMIR) or when observations
taken at widely different dates are combined. It is
planned to also use the barycentric reference in the
future for NOEMA.
COMPUTERS & SOFTWARE
The prototype continuum arrays GISMO and NIKA
have been better integrated into the telescope
control system NCS, which now offers functions
which are specific for these instruments. The limits
for several observing modes were reviewed and
unified, in particular for the on-the-fly drift speed
in LISSAJOUS, OTFMAP and POINTING. For NIKA,
we introduced a special “tune” subscan type as
an experimental feature. This allows, for example,
antenna TIPs (“skydips”) with an internal adjustment
of NIKA at each elevation step.
In close collaboration with the GILDAS group in
Grenoble, we have started work on a new calibration
software package, MRTCAL, which will eventually
replace the current software MIRA. And to support
data processing of NIKA data, we have developed a
new version of the raw data format IMBfits.
The TAPAS header database has been up and
running since October 2009. Observation header
data are continuously being transferred to this
database without delay. After a proprietary period
of 1 year a subset of these header data is regularly
being transferred to the Centre des Données
astronomiques de Strasbourg (CDS). In 2012, new
functionality has been added to TAPAS. Observers
can now use it as a logbook and enter comments
to individual scans. Monitoring of the system
performance has become a lot easier via new web
forms and plots of e.g. the telescope pointing
corrections, the receiver temperatures, and other
calibration parameters like the derived sky opacities.
In addition to TAPAS, we are maintaining an internal
project archive of all observational data. It contains
the results of the online data processing, i.e. the 30m
CLASS files of EMIR and HERA, and the FITS data files
of GISMO and NIKA. The archive currently contains
19
20
all data since 2009, while older data are being
added. During a limited time of one year, observers
can access their project data online. This allows, for
example, to quickly recalibrate data and retrieve
project files for rescheduled projects.
Several measures have been taken to improve the
computer network at IRAM/Granada. All network
switches at the observatory have been replaced.
The receivers and backends are now connected
with optical cables to the central switch. In case
of problems with an optical link, the switches
automatically use twisted pair cables instead. A
separate network switch has been installed in the
receiver room for guest instruments like e.g. GISMO.
This separates the instrument-specific network
traffic from time-critical network traffic related to
the control of the antenna. A 100Mbit/s radio-link is
used to connect the observatory and the offices in
Granada. We now offer WLAN in these offices and in
all visitor rooms.
Annual report 2012
21
A.Rambaud / IRAM.
Plateau de Bure interferometer
As in previous years, the 2012 operation of the
Plateau de Bure Interferometer has been smooth
on the whole. The instruments provided images
of stunning quality and resolution suitable for
the investigation of a wide range of cutting edge
science.
The interferometer performed according to
expectations with almost no downtime due to
hardware upgrades, maintenance operations and
work in preparation of NOEMA. The receivers and
the antennas all worked well throughout the year.
Scientific observations were performed in periods
of excellent phase stability and atmospheric
transparency in winter and autumn, but faced
somewhat less favorable conditions in spring and
summer, as in 2011. The recent move to the A
configuration was deferred to January 09, 2013, and
was so accomplished about two weeks earlier than
in the winter 2011 / 2012 and about one week later
than in the winter 2010 /2011. As in previous years,
the scheduling of the A configuration was readjusted
shortly after the beginning of the winter scheduling
period to optimize the observing of A-rated projects
with respect to Sun avoidance limitations and
weather constraints.
As in previous years, the percentage of contiguous
array-correlation-time scheduled for observing
programs was on average 50% of the total time.
Additional 20% have to be accounted for receiver
tuning, related checks and other unavoidable
observational overheads, array configuration
changes, interferometer upgrades, surface
adjustments and antenna maintenance; the
remaining 30% were lost because of precipitation,
wind and inadequate atmospheric phase stability.
The Program Committee met twice in 2012, around
four weeks after the proposal submission deadlines,
reviewed 203 proposals and recommended the
approval of 128 proposals corresponding to 327
individual projects. In total, more than 230 different
projects were scheduled at the Observatory in 2012,
including 4 Large Programs, 7 proposals for Director’s
Discretionary time and the backlog of projects from
Plateau de Bure observing
time and atmospheric water
vapor statistics over the
last ten years. The overall
correlation time accounts
for 49% of the total time
in the year 2012. Band 3
(200 – 268 GHz) and band 4
(275 – 373 GHz) programs
and observations in the most
extended (AB) configurations
are for the most part carried
out in the winter months.
The smooth increase in the
observing efficiency over
the years 2003-2012 results
from a combination of
weather statistics, technical
improvements and reduced
calibration overheads. Science
operations were suspended
in the autumn of 2006 for the
installation of new receivers.
22
2011. The weight on extragalactic high-redshift
research was considerable; the requested observing
time was about 3-4 times higher than the time
requested for each, nearby galaxies and young stellar
objects. Also, a fairly large amount of observing time
was invested in D-configuration between spring and
fall in the detection of line-emission from molecular
(e.g. carbon-monoxide, water) and atomic transitions
(e.g. carbon, ionized nitrogen) in galaxies at high
redshift. Annex I details all the proposals to which
time was granted in the course of the year, and the
list of projects testifies to the high scientific return of
the Plateau de Bure Interferometer.
VLBI NEWS
Both Plateau de Bure and Pico Veleta participated in
the Global VLBI session of May 2012, which observed
four projects. Due to meteorological limitations, Pico
Veleta observed 53.2% and Plateau de Bure 48.1%
of all scheduled observations (Bure did 52.3% of the
observations without sun avoidance constraints).
During a bad weather period, the Pico Veleta
hydrogen maser EFOS-10 suffered a temporary
out-of-lock. No observing time was lost due to this,
but in summer the maser was sent to T4Science,
Neuchâtel for a revision and subsequent monitoring.
The autumn GMVA session was cancelled in 2012,
so the absence of the maser was tolerable. However,
a submitted and accepted VLBI 1mm proposal for
Spring 2013 would have suffered from the absence
of a high stability frequency standard on Pico Veleta.
MPIfR Bonn kindly agreed to finance a rental maser
until the return of EFOS-10.
ONGOING WORK AND ACTIVITIES
A number of investigations and developments took
place in 2012 that deserve to be mentioned:
Inspection of the subreflector
of a Plateau de Bure antenna
during regular maintenance
operations.
In the frame of the NOEMA project, we investigated
the possibility to have a common LO reference
signal for band 2 (129 GHz to 174 GHz) and band
3 (200 GHz to 268 GHz) receivers. For this purpose,
a waveguide switching system was installed on
antenna 1, in between the Gunn oscillator module
and the band2/band3 frequency multipliers,
and its performance evaluated over a period of
several months. The results validated the use of the
waveguide switch and led to the decision to equip
all NOEMA antennas with it.
To reduce the ripple levels in the IF outputs of the
band1, band2 and band3 receivers of all six antennas,
an experimental study was carried out in September
on antenna 1 that consisted in the replacement of
the six entrance windows of the receiver cryostat
i.e. all four bands and the two 15K stages, and the
associated infrared filters. It was found that changes
made to the receiver optics had not lived up to
expectations, and that further work is necessary to
fully meet this objective.
To prepare for the arrival of the NOEMA antennas,
it was decided to renovate the control servo drive
system of one antenna, monitor its performance over
a period of several months, and validate the usability
of the prototype system. The renovation work was
carried out at the end of the summer maintenance
period on antenna 5 and consisted in the
replacement of the azimuth and elevation motors,
in the refurbishment of the closed-loop feedback
systems, and in the modernization of the control
software. Due to technical difficulties and scheduling
issues it has not been possible to compare and
validate the performance of the new system before
the end of 2012. The final evaluation is expected to
take place in the spring of 2013.
As in previous years, the surface quality of all of the
antennas was verified by means of holographic
measurements at the end of the maintenance
period. Surface panels were readjusted when
deemed necessary. The final overall surface precision
achieved by holography was 35μm (weighted by
Annual report 2012
23
illumination) for antenna 1 and better than 45μm for
all other antennas.
In the frame of the observatory’s antenna surface
improvement program, a significant effort was made
in the maintenance period 2011 on replacing the
central struts of the ring 2 to ring 6 panels of antenna
6. These panels are known to stress and deform in
conditions of a significant thermal gradient between
the central supporting strut (5th point) and the set
of corners struts. To eliminate this misbehavior and
contain surface efficiency losses within allowable
tolerances, all central struts were replaced with a set
of thermal gradient compensating struts. After more
than one year of operation with the new struts and
regular monitoring of the panels surface precision by
holographic techniques, we feel confident that we
have succeeded in correcting the problem.
To address the maintenance issue associated with
the arrival of new antennas and related to displacing
individual antennas on the east-west and northsouth tracks from a remote position to inside the
hangar, it was decided to add two sidetracks, one
on the east (E 12) and one on the west (W 05) track.
The construction of these two sidetracks, which will
reduce the number antenna displacements and the
associated expenditure of time and effort, has started
in the summer of 2012 and is scheduled to achieve
completion in the summer of 2013. During summer
the STM Pugnat company completed contracted
work, which started in 2010 and continued in 2011,
to repair and resurface the pavement with concrete
in between the rails along the east-west and north
south tracks.
In the spring of 2014 Plateau de Bure’s Science
Operations Group (SOG) will be in the forefront of an
institute-wide effort to validate the characteristics of
the seventh antenna. To prepare for this major effort,
support future antenna maintenance operations
and provide an additional powerful platform to test
software, a new mode of operation was developed
that allows the control of two independent antenna
sub-arrays. While one sub-array would operate in
science mode to address and meet the needs of
the astronomical community, the second subarray would be set up to test and validate novel
and upgraded equipment and software. First
observations with the current six-element array in
the so-called double-array mode were successful
but to fully assess and implement the new operating
modes a continuation of this development effort is
being planned for the spring of 2013.
Plateau de Bure’s phase switching (180°) and
sideband separating (90°) scheme is based on a
32-element set of Walsh functions. The same set of
functions will be available for the NOEMA array. To
prepare for the arrival of the new antennas while
building on the experience with the six-element
array, a study was conducted that investigates
the optimum choice of Walsh code sequences for
NOEMA’s 12-antenna array. An optimization was
performed that yields the highest phase-switching
frequency and simultaneously produces the smallest
summed squares of crosstalk. We plan to implement
the new sets of Walsh functions for the arrival of the
seventh antenna.
The radiometers on the Plateau de Bure have
operated without major problems. Minor
disturbances like two 15V power supply failures and
a defective load arm were quickly resolved. In the
context of the NOEMA project, plans for an upgraded
multi-channel radiometer are under development.
With the continuous and rapid developments in
wireless services and satellite communication, more
and more sources of radio frequency interference
(RFI) are found to operate in the millimeter range. To
spot and locate new sources of RFI in the frequency
range covered by the 22 GHz radiometers and to be
able to react accordingly, we have set up a prototype
interference monitoring system. The system uses a
wide-band spectrum analyzer connected to the IF
output of the radiometer to record spurious changes
in the power levels of adjacent spectral channels. The
prototype, which operates across the 19 to 26 GHz
RF-band of the radiometers, was installed on antenna
5. The system is presently undergoing testing.
The pointing accuracy of the Plateau de Bure
antenna is limited by thermal gradients in the
antenna structure and by changes in the antenna
Sidetrack construction and
pavement refurbishment work
on the western track, as of June
05, 2012.
24
inclination. The latter appear to be linked to
positional instabilities of the station on which the
antenna is clamped. To correct for these changes,
the inclination of every antenna is continuously
measured with a high-precision (1”) dual-axis
tiltmeter placed in the antenna yoke at the high
end of the azimuth axis. With the disappearance
of Leica’s NIVEL-20 tilt-meters from the market and
the arrival of new antennas, we have started a
monitoring program to evaluate the performance
of a competitive tiltmeter manufactured by Jewell
Instruments. According to the results of the
investigations, the new tiltmeter are fully adapted to
needs and will equip the NOEMA antennas.
During the regular operations of the cold-heads
maintenance 2011, the vertical polarization of the
band 4 mixer (275 to 373 GHz) on the receiving
system of antenna 4 had gone open-circuit. This fault
was cleared during the antenna maintenance period
of 2012. In parallel, it was necessary to replace the
band 2 (129 GHz to 174 GHz) LO frequency doublermodules in two antennas, as they began to show
signs of fatigue.
USER SUPPORT
The Plateau de Bure Science Operations Group (SOG)
is staffed with astronomers that regularly act as
astronomers on duty to optimise the scientific return
of the instrument, directly on the site or remotely
from Grenoble, provide technical support and
expertise on the Plateau de Bure interferometer to
investigators and visiting astronomers for questions
related to the calibration, pipeline-processing and
archiving of Plateau de Bure data, interact with
the scientific software development group for
developments related to the long-term future of the
interferometer, perform the technical reviewing of
the proposals, and collaborate with technical groups
to ensure that operational requirements are being
met. Six astronomers were appointed to the group at
the beginning of 2012.
SOG members holding their
weekly meeting with a video
call to the Observatory
As in previous years, work was continued in the
context of extending and improving the Plateau de
Bure data calibration pipeline. In 2012, efforts were
directed to improve the pipeline’s robustness, refine
the antenna-based RF passband calibration, ensure
consistent phase calibrations in both the horizontal
and vertical polarization, and release an automatic
assessment routine for projects aiming at detecting a
weak emission line and continuum. In parallel, work
was made to improve the accuracy of the absolute
flux calibration scheme. An effort was directed to
narrowing down antenna gain factors: visibilities
of the radio source MWC 349 are now fitted to a
frequency- and size-dependent, modelled visibility
function. Another effort was started on modelling
the mm-SED of the optically thick core surrounding
LkHa101. The aim is to calibrate it better than a few
percent and thereby establish an alternative highprecision flux calibration reference to MWC 349.
In 2012 assistance was given to 34 investigators from
Europe and overseas visiting IRAM Grenoble for a
total of 139 days to reduce data from the Plateau de
Bure Interferometer. Advice and support was also
provided to a number of experienced astronomers
from Caltech/Pasadena, CSPF/Copenhagen, ESO/
Garching, MPIA/Heidelberg, LERMA/Paris and EPFL
Geneva for a total of 51 days to reduce and analyze
Plateau de Bure Interferometer data remotely from
their home institutes. Assistance was provided to 58
projects in total. IRAM astronomers collaborated on
69 projects in which they were directly involved.
As in previous years, in a continuing and successful
effort with the Centre de Données astronomiques
de Strasbourg (CDS), data headers of observations
carried out with the Plateau de Bure Interferometer
are conjointly archived at the CDS, and are available
for viewing via the CDS search tools. In 2012,
the archive contained coordinates, on-source
integration time, frequencies, observing modes, array
configurations, project identification codes, etc. for
observations carried out in the period from January
1990 to September 2011. The archive is updated at
the CDS every 6 months (May and October) and with
a delay of 12 months from the end of a scheduling
semester in which a project is observed in order to
keep some pieces of information confidential until
that time.
Annual report 2012
25
RADIONET USERS
As in 2011, travel funds have been made available
to RadioNet eligible astronomers from non-IRAM
partner countries for expenses incurred during
their stay at IRAM for reducing data from the
Plateau de Bure Interferometer. These funds, which
were initially made available by the European
Commission for the institutes participating in the
FP 6 TransNational Access (TNA) initiative, are today
granted by the FP 7 program. Because of budget
restrictions in the RadioNet program, only expenses
related to accommodation or travel were covered
in 2012. For the same year, the Program Committee
received 42 eligible proposals (25% more than in
2011) and recommended 22 proposals (5 A-rated,
17 B-rated) for observations with the Plateau de
Bure Interferometer. Taking into account proposals
accepted in 2011 but continued in 2012, time was
allocated to 17 eligible proposals corresponding to a
total of 25 projects and 325 hours of observing time.
Since the beginning of RadioNet, access time was
allocated to 112 eligible proposals (12 in 2004, 11 in
2005, 11 in 2006, 13 in 2007, 14 in 2008, 6 in 2009,
14 in 2010 and 14 in 2011) for observations with the
Plateau de Bure Interferometer, corresponding to a
total of ~2500 hours (272 in 2004, 239 in 2005, 272
in 2006, 326 hours in 2007, 334 in 2008, 140 in 2009,
266 in 2010 and 327 in 2011) of observing time.
User responses to questionnaires of the European
Commission and to the RadioNet management
in Bonn show that IRAM continues to maintain an
excellent reputation concerning the assistance
and service given by scientists and support staff to
visiting astronomers.
RadioNet observing time was
allocated to eligible principal
investigators from United
Kingdom (percentage of total
time is 52%), Italy (32.8%), the
Netherlands (5.6%), Sweden
(3.8%), Denmark (2.6%),
Austria (1.3%), Hungary
(1.0%), Portugal (0.6%), and
Switzerland (0.3%) with
a balanced distribution
between PhD students and
post-doctoral researchers
(51%) and senior scientists
(49%).
26
Grenoble Headquarters
FRONTEND GROUP
The IRAM Front End Group had a busy year in 2012
with maintenance, upgrade and development
activities for both NOEMA and the 30 m telescope,
as well as for the upgrade of the laboratory
instrumentation and the development and tests
of prototype receiver and components for the
European AMSTAR+/AETHER collaboration and the
ALMA Band 2&3 projects. The year 2012 also marked
the end of the ALMA Band 7 cartridge production,
totalling 73 cold cartridge assemblies delivered from
IRAM to the ALMA project.
DEVELOPMENT OF NOEMA FRONTEND
The NOEMA Front-Ends specification requires a redesign of the current PdBI Front-Ends, which have
been in continuous operation since their installation
in 2006. The design of the NOEMA Front-Ends has
started in collaboration with the IRAM Mechanical
Group. Such Front-Ends will be state-of-the-art
dual-polarization quadri-band heterodyne receivers
based on SIS superconducting mixers that cover the
3 mm (Band 1), 2 mm (Band 2), 1.3 mm (Band 3) and
0.8 mm (Band 4) bands using a sideband separating
(2SB) mixer technology with two 7.744 GHz wide
(3.872-11.616 GHz) IF bands per polarization.
Therefore, the Single Side Band (SSB) backshort-
Current PdBI receiver
specification and NOEMA 2SB
receiver specification.
Current PdBI receivers
2SB NOEMA receivers
Band
RF [GHz]
Mixer
scheme
IF
[GHz]
1
83-116
SSB
4-8
2
129-174
SSB
3
200-268
4
277-371
Notes
RF [GHz]
IF [GHz]
Backshort
tuning
78-116
3.872-11.616
RF band extension down
to 72 GHz under study
4-8
Backshort
tuning
127-179
3.872-11.616
New mixer with
integrated IF
superconducting hybrid
SSB
4-8
Backshort
tuning
200-276
3.872-11.616
EMIR E2 type 2SB
mixer with permanent
magnets
2SB
4-8
One IF
used
275-373
3.872-11.616
ALMA Band 7 mixer chip
and integrated IF hybrid
tuned SIS mixers delivering 4 GHz IF bandwidth per
polarization channel, which is currently adopted
for PdBI Bands 1-2-3, will be upgraded to the 2SB
technology delivering two 7.744 GHz wide IF band
per polarization channel. Also, the four RF bands of
the NOEMA receivers will be slightly larger than the
ones of the current receiver generation. The main
NOEMA Front End specifications are given in the
following table.
The two main goals of the Front-End Group during
the coming years are to build four new receivers
for the four new NOEMA antennas (Phase A of the
project) and to upgrade the six PdBI receivers to the
NOEMA specification.
Notes
A view of the inner part of the NOEMA Front-End,
with two out of the four bands, is shown in the
following Figure.
Annual report 2012
27
CRYOGENIC OPTICS MODULES
The first prototype of NOEMA cryogenic optics
module was designed and fabricated for Band 3
(200-276 GHz). It comprises two ellipsoidal mirrors
thermalized at 15 K, as well as a polarization splitting
wire grid and two single-polarization broad-band
feed-horns which will be maintained at 4 K. The
various parts are supported by a 6060 Aluminium
frame and use G 11 fiberglass tabs to thermally split
the 15 K optics and the 4 K parts. Unlike the current
generation PdBI cryogenic optics modules, the new
design allows to keep the module assembled after
its room temperature tests on the antenna range,
before its final integration into the receiver cryostat.
The design of the different parts of the module was
also simplified to ensure a better alignment on the
sky between the two receiver polarizations. We will
adopt this same design philosophy for the cryogenic
optics modules of NOEMA Band 1 and 2.
Inner view of the NOEMA
cryostat showing the 15 K
plate on which the four RF
cryogenic modules will be
mounted (only the modules
for Band 2 and Band 3 are
shown). Two of the RF beams
(4 w at the lowest frequency
edge of the band) are also
shown.
2SB SIS MIXERS
After the successful experimental results obtained
with the EMIR E2 2SB mixer in 2011, and after that
mixer proved to work reliably in the 30 m antenna,
we decided to adopt the same type of mixer for
NOEMA Band 3; the mixer required only slight
modifications to the mechanical blocks.
After a decision was made to specify the NOEMA
IF band across 3.872-11.616 GHz, some key
components of the IF chain required some slight
modification with respect to those operating over
the more standard 4-12 GHz band (used for example
for the ALMA Band 9&10 IFs). In particular, new
prototypes of cryogenic isolators and IF cryogenic
PLATEAU DE BURE INTERFEROMETER MAINTENANCE AND NEW TEST EQUIPMENT
MAINTENANCE
The maintenance work concerned the Sumitomo cryogenerators,
which took place during the summer period. Starting from
2012, the maintenance of the cryogenerators is regularly made,
approximately every 15000 hours of operation. The on-site
intervention uses the “hot-swap” method, which consists in
changing the active parts of the cold heads without removing
the cryostat from the receiver cabin. The three cold-heads
installed on Ants. #1, #3, and #6 were hot-swapped, then sent
to Sumitomo-Germany for servicing. On Ant. #4, the Band 4
(275-373 GHz) receiver module that had a SIS mixer chip in short
circuit (in Pol H) since September 2011 was swapped with a spare
one. This spare module had been previously characterized in
the laboratory. A maintenance work was made on the 22 GHz
Water Vapour Radiometers on Ant. #2 (room temperature load
measurement was repaired) and on Ant. #6 (the radiometer was
serviced after a water leakage into the cabin due to weathering).
A number of Local Oscillator (LO) systems were repaired following
failure of Gunn oscillators, attenuators and frequency doublers.
The HDPE vacuum windows and IR Teflon filters of the four PdBI
receiver bands on Ant. #1 were swapped with new broader band
ones having corrugations similar to those mounted in the Pico
Veleta EMIR receiver. The goal is to understand and try to improve
the problem of ripple in the measured noise temperature across
the 4-8 GHz IF frequency.
NEW TEST EQUIPMENT AT THE SITE
A waveguide switch that drives a LO signal to either the Band 2
or the Band 3 SIS receiver modules was tested in the laboratory
and then installed on Ant. #1 in October 2012. The role of this
WR12 waveguide switch is to deliver a monochromatic LO
signal across the 69.3-88.1 GHz frequency band generated by
a common Gunn oscillator to either the frequency doubler of
the Band 2 receiver or to the frequency tripler of the Band 3
receiver. Site tests with the PdBI interferometer were started to
verify if such switch, situated outside the PLL loop which locks
the fundamental oscillator frequency from the Gunn module,
worked well and could be adopted for NOEMA. This would allow
replacement of the two 69.3-88.1 GHz Gunn LO systems that
independently drive the Band 2 and Band 3 receiver modules by
a single Gunn LO system cascaded with the switched waveguide.
A radio frequency interference (RFI) monitoring system for the 1826.5 GHz band was installed on Ant. #5. The system is based on a
spectrum analyser (Textronix 492BP) connected to the 2-10 GHz
IF monitor output of the water vapour radiometer and was set to
detect spurious signals across 18-26.5 GHz over –110 dBm at the
radiometer input using a 3 MHz bandwidth. A lower frequency
low-cost rack mounted spectrum analyzers (from Aaronia) was
also tested in the laboratory. It was found to be suitable for the
direct detection of RFI disturbances of up to 9.4 GHz and across
most of the IF frequency band from the 18-26.5 WVR through its
IF monitor output. This low-cost analyser should replace the most
expensive one.
28
low noise amplifiers covering 3.8-11.7 GHz were
developed by external institutes and validated to
work well for the NOEMA Front-End. Laboratory test
results demonstrated that the NOEMA Band 3 mixers,
which delivers two 3.872-11.616 GHz IF bands,
perform as well as the EMIR E2 mixer, which delivers
two similar IF bands across 4-12 GHz.
We also focused our developments on the mixer
for NOEMA Band 2. An IF coupler chip covering the
4-12 GHz frequency range (also suitable for 3.8-11.7
GHz) was developed. The design is based on three
coupling sections using superconducting striplines.
The simulated performances of the chip are shown
below.
The great advantage of this IF chip compared to
commercially available couplers is its planar design,
which makes it suitable for integration with the
mixer chip into the mixer block, so resulting in one
very small 2SB mixer unit. This is especially useful for
multipixel receivers.
The new NOEMA Band 2 SIS mixer makes already use
of this new IF coupler chip (see following figure).
The NOEMA Band 1 SIS mixer, still to be developed,
will also integrate this new IF coupler. Such mixer will
employ SIS chips identical to those installed on the
EMIR E 0 band.
Left: Photo of the IF
superconducting hybrid
installed in a connectorized
block. Right: One half
of the new Band 2 2SB
mixer with integrated IF
superconducting coupler.
BIAS ELECTRONICS MODULES AND CONTROL BOARDS
New bias electronics modules and control boards
based on EtherCAT are under development. These
include: 1) a module (see Figure below) capable
of biasing the 16 SIS junctions of the mixers of all
NOEMA bands; 2) a module for biasing the cryogenic
low noise amplifiers; 3) a control board for the warm
IF chain and the IF laser link.
A new temperature reading module is also under
development.
The design of the fully electronically tuneable
85.744-108.256 GHz NOEMA Band 1 Local Oscillator
(LO) prototype was completed. The LO rack shown
in the Figure below includes a 14.29-18.04 GHz YIG
oscillator cascaded by an Active Multiplier Chain
(AMC) predicted to deliver a minimum output power
of 6 dBm across the 85.744-108.256 GHz band at the
Power Amplifier (PA) input. The PA is followed by a 3
dB recombination coupler which delivers between
12 and 17 dBm output power. A fraction of the AMC
output signal is sent to an harmonic mixer, which
is pumped by a 13.2-16.4 GHz reference signal,
Annual report 2012
29
Inner view of the NOEMA
Band 1 (85.744-108.256 GHz)
LO rack.
and outputs a 100 MHz IF. The 100 MHz IF beat is
compared with a 100 MHz second reference in the
PLL to lock the YIG. The bias cards and the PLL are
remotely controlled using CAN module interfaces.
The details of the AMC, the PA and the 3 dB coupler
are shown in the Figure below. The PA and the 3
dB coupler are presented in reverse position (and
slightly shifted one to another) compared to the
AMC to show the details of the MMICs implantation.
In the AMC, the 14.29-18.04 GHz input signal coming
from the YIG oscillator goes through a 28.58-36.08
GHz frequency doubler, an amplifier, a band pass
filter, and a frequency tripler. At the tripler output,
the 85.744-108.256 GHz signal is amplified and
filtered by a pass-band filter and pass through a
WR10 waveguide using a waveguide to microstrip
line transition. A fraction of the AMC output signal
pass through a -10 dB coupler and is sent to the PLL
output which is connected outside with the PLL
harmonic mixer. The AMC output signal is split by a
3dB hybrid coupler and amplified in the PA module.
The two PA outputs are then recombined by a
second 3 dB hybrid coupler. This hybrid arrangement
optimizes the saturated power level and the output
return loss.
Details of the Active
Multiplier Chain (AMC1), of
the Power Amplifier (PA 1)
and of the 3 dB coupler
which are parts of the
NOEMA 85.744-108.256 GHz
Local Oscillator system.
30
UPGRADES AND NEW DEVELOPMENTS FOR PICO VELETA
No maintenance was needed in 2012, neither for the
EMIR quadri-band receiver nor for the HERA 1 mm
multibeam receiver.
The performance of the 1.3 mm band E 2 2SB SIS
mixer installed last year on EMIR was monitored
throughout 2012. The miniature permanent magnets
used in that mixer proved to reliably suppress the
Josephson currents through the superconducting
SIS junctions also in the antenna electromagnetic
environment. Following this successful result, it was
decided to adopt the same type of mixer also for
NOEMA Band 3.
UPGRADE OF HOLOGRAPHY RECEIVER
The 39.592 GHz dual channel holography receiver
built in 1996 for the measurement of the 30 meter
Pico-Veleta telescope surface was upgraded. That
receiver employed the Right Hand Circular (RHC)
polarized source signal from the now obsolete
ITALSAT satellite. The receiver was upgraded to
work with the 45 degrees linear polarized signal at
39.402 GHz emitted by the ALPHASAT TDP 5 satellite
module. The satellite is scheduled to be launched in
July 2013 and to start broadcasting in Autumn 2013.
The local oscillators which match the new beacon
frequency and the 45 degrees R&L waveguide twists
were provided to IRAM-Granada for the installation in
the receiver and in the mountain transmitter.
3 MM BAND MULTIBEAM RECEIVER FOR THE 30M TELESCOPE
Good progress was made on the design of a 5x5
pixels dual-polarization 2SB SIS receiver for the 3 mm
band. The receiver baseline design utilizes only
one of the two output sidebands per polarization
channel and delivers a total of 2 pols x 25 pixels = 50
IF channels, each covering 4-8 GHz instantaneous
band. The receiver design allows observation at
different sky frequencies on the two polarization
channels thanks to the use of two independent local
oscillators that can drive the SIS mixers to different
frequencies.
5-PIXEL DUAL POLARIZATION LINEAR-ARRAY MODULE
One important milestone for this project is the
development of a 5-pixel dual polarization linear
array prototype module, which will be replicated for
the construction of the full 5 x 5 pixels receiver RF
Mechanical drawing of the
5-pixel dual polarization
linear array prototype
module including the feedhorns, the OMTs, the LO
coupler and RF hybrids and
the low noise amplifiers.
module. The design of the 5-pixel linear array module
is shown in the Figure.
Annual report 2012
31
WIDEBAND ORTHOMODE TRANSDUCER
A waveguide Ortho Mode Transducer (OMT)
was designed to separate two incoming linear
polarization signals across a very broadband. The
OMT development is common to the 3 mm multibeam receiver and to the ESO supported ALMA Band
2&3 study in which the IRAM Front-End Group is
involved. This OMT, based on a waveguide turnstile
junction, was optimized to cover 67-116 GHz, i.e. the
ALMA Band 2 (67-90 GHz) and Band 3 (84-116 GHz)
combined. This is a challenging project because
of the large relative operation bandwidth of the
component, which is close to ~54%. Six of these
OMTs are being manufactured via electroforming
process of Aluminum mandrels (see Figure below,
left panel). This design stands on the development of
a previous version of such OMT prototype, designed
to cover the slightly narrower 70-116 GHz band,
which was fabricated and tested. The electroformed
OMT unit and its performance measured with the
IRAM millimeter vector network analyzer are shown
respectively, on the Figures of the central and right
panels. That first OMT version performs well and has
input reflection of below –17 dB, cross-polarization
level of below –35 dB, and insertion losses of order
–0.25 dB at room temperature. We expect the newer
design to have even lower input reflection and to
work down to 67 GHz.
Left: Electroformed OMT
designed to cover 70116 GHz. Right: Measurement
results of 70-116 GHz OMT.
RF HYBRID AND LO DISTRIBUTION COUPLERS
A 1-pixel prototype of a broadband RF hybrid
coupler combined to a LO distribution coupler was
designed, manufactured and tested. This component
consists of three blocks comprising two waveguide
circuitries split on opposite sides of a thin block
which is sandwiched between two external blocks
1-pixel RF hybrid and LO
coupler. Left: Exploded
view of the designed
unit. Center: Assembled
prototype fabricated at IRAM.
Right: Disassembled parts
showing the two sides of the
central part of the unit (RF
waveguide input on the left
side, LO waveguide input on
the right side).
Measured performances of
the broadband RF hybrid
coupler on IRAM millimeter
Vector Network Analyzer.
32
(see Figure). The unit combines different waveguide
technologies: the coupling between the LO and the
RF signals is achieved by circular holes on the narrow
waveguide side, whereas the 3 dB RF hybrid coupling
is obtained through branch lines. This component
operates across a very wide band, 70-116 GHz.
Two prototypes of this component were
manufactured and tested using the IRAM millimeter
vector network analyzer. The measured amplitude
imbalance is +/-0.7dB and the measured phase
imbalance is of +/-1 degree across the full 70-116
GHz range, with an input reflection of below –20 dB.
LO AND RF COUPLING DISTRIBUTION FOR 5 PIXELS
The design of the combined LO and RF coupling
distribution for 5 pixels, which enables the possibility
of using a single local oscillator to pump the 25
pixels array per polarization channel is shown in
following figure. Slight differences in the five branch
lines coupling regions of the LO signal allow to
compensate for the losses along the LO path. As
for the 1-pixel prototype, the coupling between
the LO and the RF waveguides is obtained through
waveguide holes. The simulated electromagnetic
performance of the LO distribution to the five pixels
predict a maximum difference in the LO coupling
values to the RF waveguides of only 1.5 dB.
Waveguide path for the LO
distribution into a 5 pixel
linear array combined to
the RF hybrid coupling for
5 pixels. The RF signal is
distributed through the
waveguides visible on the
bottom, while the LO signal
is distributed through the
waveguide visible on the top.
The three MVNA Test-Sets
extenders with the AMC
power source, the Agilent
N5244A PNAX and the power
supply.
MILLIMETER-WAVE VECTOR NETWORK ANALYZER
EXTENSION MODULES
We developed three millimeter-wave extension
modules for a commercial Vector Network Analyzer
(VNA) to cover the 70-279 GHz in 3 MVNA bands (see
table below). Such development complements the
260-375 GHz extender built in the past and allows
the IRAM S-parameter measurement capabilities to
span across all the frequency range covered by the
NOEMA Front Ends. The Band 2 and Band 3 MVNA
extension modules combine a 65-90 GHz high
power source (an Active-Multiplier-Chain) and two
through-reflect test-sets allowing through-reflect
scattering parameters measurement. The Band
1 extension module is a full two-port scattering
parameter measurement system with two throughreflect modules. Each Band 1 extension module
includes a passive harmonic multiplier used as
millimeter source. The extenders are connected to an
Agilent N5244A PNAX which drives the RF and the LO
frequency in the range of 8 to 29.6 GHz according to
Annual report 2012
the used band. Most of the devices, used in the test
sets (like the mechanical box, the Schottky harmonic
mixers, the waveguide couplers and the kit of
calibration standards) were built in house.
Band
#
Frequency Band
[GHz]
Transmission
dynamic [dB]
Reflection
dynamic [dB]
1
70-116
80
50-60
2
127-179
80-100
60
3
200-278
90-100
60
33
COMPLETION OF ALMA BAND 7 CARTRIDGE PRODUCTION
In December 2012, the ALMA Band 7 (275-373 GHz)
cartridge production was successfully completed
within cost and allocated timescale.
In 2012, four retrofitted pre-production cartridges
and the last 13 production cartridges were
assembled, tested and delivered to the ALMA
project. Ten spare 2SB mixer assemblies were also
fabricated and tested. One of the cartridge test set
was reworked prior to its shipment to the ALMA
Operation Support Facility (OSF) in Chile.
A first cartridge maintenance training was provided
to our Chilean colleagues in June 2012.
The following Figures show the integrated noise
temperature and the image band suppression of
the 65 production cartridges.
Integrated SSB receiver
noise temperature (left) and
image band suppression
(right) for all 65 ALMA Band
7 production cartridges (#9
to #73).
AMSTAR+ / AETHER ACTIVITIES
Within the framework of the AMSTAR+ FP7
programme, a collaborative effort of a number of
European research institutes which ended in June
2012, IRAM was involved in the two following tasks:
Task 1: the development of a prototype pixel
for a W-band dual polarization module using
metamorphic HEMT technology to be integrated
into a Focal Plane Array;
TasK 2: the development of advanced receiver pixels
and LOs for large Focal Plane Arrays in the near mmwave domain.
The European programme is continuing through the
new AETHER project, which started in July 2012.
AMSTAR+ TASK 1
Waveguide W-band Low Noise Amplifier (LNA)
modules integrating metamorphic MMIC amplifiers
that were designed and fabricated at IAF (Fraunhofer
Institute, Freiburg, Germany) were developed at
IRAM in 2012. The mechanical packaging of the
W-band LNA integrates the following components:
a) one IAF MMIC amplifier; b) two probe chips
(waveguide-to-coplanar waveguide CPW
transitions); c) one bias board circuit; and d) one DC
bias connector from Microtech. Views of a packaged
MMIC amplifier and of its internal details are shown
in the Figures below.
A number of W-band LNA modules were built and
characterized (see Figure below, left panel). The
external dimensions of the W-band LNA module
were chosen to allow assembly of two LNA units
Left: LNA base block (cover
block removed) showing the
input and output waveguides
and DC bias board. Right:
IAF MMIC glued to LNA
base block in between two
waveguide-to-CPW quartz
probe chips.
34
with the waveguide orthomode transducer (OMT),
which was also built and tested at IRAM. A complete
dual linear polarization module including two LNA
units per polarization channel interconnected
through a commercial isolator was built and
characterized (see Figure below, right panel).
A cryostat equipped with the AMSTAR+ module was
installed on the IRAM Pico Veleta 30 m telescope and
its performance were measured in July 2012. A full
3 mm band (84-116 GHz) spectrum was taken on
IRC+10216 in less than an hour (see Figure below)
using the AMSTAR+ prototype receiver and the Fast
Fourier-Transform backends (FTS), showing a very
The amplifiers were first characterized at room
temperature, then at cryogenic temperature.
The results of the characterization of one of the
amplifiers are presented on the Figure below.
good baseline and no contamination from lines
on the image sideband. A longer integration time
spectrum, taken on the same source, shows the RMS
noise closely follows the radiometric noise limit.
Allan variance analysis gives results similar to other
IRAM SIS receivers.
Left: some of the W-band
LNA modules packaged and
tested at IRAM. Right: spectral
line survey conducted with
AMSTAR+ receiver module
installed on the IRAM 30 m
telescope.
Left: Room temperature
S-parameters measurement
of one of the W-band LNAs
performed with the IRAM mmwave Vector Network Analyzer
across 70-116 GHz. Right:
Noise temperature and gain of
W-band LNA at 4.2 K.
AMSTAR+ TASK 2
A small footprint 2SB mixer module for the 200-280
GHz frequency range, having a flat noise response
over the 4-12 GHz IF band, had successfully
developed at IRAM in 2011 and is currently mounted
on the E2 channel of the EMIR receiver. Because of
the good results and the already sufficiently small
footprint of the 2SB mixer module, the initial project
of designing a 2SB mixer-on-a-chip was abandoned.
Instead, it was decided to further pursue the
integration of the 2SB mixer by designing an IF
superconducting hybrid coupler, which can be
integrated with the mixer chip into one block. Such
IF hybrid, to be employed in the NOEMA Front End,
is under development.
Additional tests of the 2SB mixer were performed
in conjunction with 4-12 GHz low noise amplifiers
(LNAs) with low input reflection coefficient
developed at Yebes. Different types of LNAs were
tested, which were based on MMIC or hybrid
transistor technologies. The results were compared
to the measurements obtained with the standard
set-up of 2SB mixer cascaded with cryogenic
isolators and classic amplifiers (which were retained
for NOEMA). The noise temperature of the receiver
without isolators was found to be slightly higher
than thenoise temperature of the receiver with
isolators. A ripple was observed in the measured
noise versus IF frequency, at the origin of the
reflections between mixer and amplifier. They ripple
was more pronounced for the case of the MMIC
LNA.
Annual report 2012
35
CONTINUUM ARRAY DEVELOPMENTS FROM THE 30M TELESCOPE
GISMO
GISMO(-1) (prototype)
Since April 2012 GISMO has begun the 2nd part
of its life: it is now in its nominal configuration and
opened to the community with a basis of 2 science
runs per year organized in observing pools of 2
weeks each. For the April 2012 and November 2012
pools the median NEFD = 13 and 18 mJy•s1 / 2, and
is dominated by sky noise. In both cases a large
fraction (~70%) of the scheduled time was lost due
to bad weather. However a majority of the projects
rms requirements were achieved.
For the 3rd pool run in April 2013, 19 projects have
been accepted. A 4th pool run is scheduled for the
autumn 2013.
An article from Staguhn et al. has been submitted
for publication to ApJ in February 2013. The map
studied, called the Gismo Deep Field (GDF), is
a portion of the GOODS-N field, containing the
detection of 12 sources, 7 of them being discoveries
without any known counterpart. This is a good
demonstration of the deep integration capacities of
GISMO for the study of the far universe.
GISMO-2 (instrument)
IRAM has been active in designing the optics for
GISMO-2, a dual band follow up of GISMO 1. It will
be a 2 band system using filled arrays at 150 and 250
GHz and covering a 4’x5’ FOV. The GISMO-2 cryostat
is now in development, as well as the TES detectors
arrays, and the optical elements including large
silicon lenses. The delivery for first tests should occur
in about one year.
NIKA
NIKA(-1) (prototype)
The 4th test run of NIKA occurred in June 2012,
the goals being the installation and test at the
new permanent position. The curved M 6 mirror
and the HDPE lenses were machined by the IRAM
mechanical workshop, with a new kind of large
band-pass anti-reflection pyramidal corrugations.
The unstable weather allowed toproduce only
calibration maps, however sufficient to witness
the modifications of several problems seen in the
previous runs.
The 5th test run occurred in November 2012. It
included the new NIKEL electronics developed
at the LPSC, and a KID auto-tuning procedure.
Unfortunately an unforeseen saturation of a cold
amplifier limited the number of pixels to 69 for the
240 GHz band. Besides, the arrays showed such
disparities that in order to appreciate the system
performances, it was worth giving 2 numbers per
band for the sensitivities: NEFD 140GHz = 31 (18)
mJy•s1 / 2 for the 101 (20 best) valid pixels
NEFD 240GHz = 81 (24) mJy•s1 / 2 for the 69 (8 best)
valid pixels
Some science observations could be conducted, in
particular on the topics of diffuse emission, and the
Sunyaev Zeldovich effect.
A change of the cold amplifier and KIDs array is
foreseen for the next run in June 2013. The camera
could then be opened to external observers on a
shared risk basis for the Winter 2013-2014.
Left: screenshot from Zemax
of the GISMO(-1) new optics;
centre: GISMO installed at
this final permanent position;
right: details of the ray
tracing inside the GISMO-2
cryostat, the optical elements
displayed are the entrance
window, the cold pupil stop,
2 folded off-axis mirrors,
the field stop, the dichroic
separating the 1.2 and 2 mm
bands, and 2 lenses for each
bands producing an excellent
image quality.
36
NIKA-2 (instrument)
The development is funded with an ANR proposal
of 900 k€, it will also benefit from a Labex Focus
(driven by IPAG), and a EU ERC granted 500 k€ to
the CEA to support polarimetry, which follows
recommendations from the SAC and led to modified
specifications accordingly. Hence the cryostat will
contain 3 channels for simultaneous observations: a
1000 pixels array for the 150 GHz band, a 2500 pixels
array for the 250 GHz band, and possibly another
2500 pixels array at 250 GHz to allow simultaneous
polarized observations. Each of these 3 arrays will
fully sample a 6.5’ FOV diameter, implying 0.75 Fλ
pixel angular size.
Left: NIKA(-1) installed at its
new permanent position;
Right: Zemax ray tracing
inside the NIKA-2 cryostat
viewed from the top (top) and
from the side (bottom), the
optical elements displayed
are the entrance window,
the cold pupil stop, 2 folded
off-axis mirrors, the field stop,
a lens, the dichroic separating
the 1.2 and 2 mm bands,
the polarizer separating
orthogonal polarizations at
1.2 mm, and 2 lenses for each
bands allowing producing an
excellent image quality on
the detector.
In the 2nd half of 2012 intense work at IRAM was
engaged for the optical design of NIKA-2. With
2.3 m long and about 900 kg, NIKA-2 will be a big
instrument. The spacing constraints in the 30m
telescope receiver cabin were analyzed, a review
meeting was scheduled in April 2013. The electronics
will be made with 20 NIKEL boards currently in
development at the LPSC. The pixel design is derived
from the LEKID arrays tested at Pico Veleta in the
NIKA(-1) prototype. Each array will be achieved on
a single 4 inches Si wafer. Several developments are
ongoing to optimise the sensitivity (e.g. AR coating,
bridges, TiN, etc.); G. Coiffard has started a PhD on
this subject in the IRAM SIS group.
The NIKA-2 arrays will be tested in laboratory
electrically and optically, using a modified NIKA‑1
cryostat, which includes an optics designed in the
summer 2012 that allows illuminating 4 inches
wafers. Thus it is possible to test the arrays while the
NIKA-2 cryostat is in fabrication. Some early tests
conducted on 1000 pixels arrays have validated the
testing facility and demonstrated performances in
line with the current 2 inches wafers.
30M CABIN MIRRORS REFURBISHMENT
The specifications updates and beginning of
development of both the bolometric project
and the heterodynes FPAs have reactivated the
project of the 30m cabin mirrors refurbishment.
The most noticeable evolution is the realization
that the structures from the 2010 propositions
were incompatible with the future instruments
sizes and locations. Another evolution was the
rationalization of the project steps, in particular
the motorization of M3 will not be necessary until
a need for more than 7’ FOV emerges. Therefore,
Screenshots from a SketchUp
model of the future large FOV
optics of the 30m telescope
cabin receiver, view from the
top (left), front (center), and
oblique (right). The future
optics systems is in green,
the current one in semitransparent brown, NIKA-2 in
white, EMIR in red, and HERA
in yellow.
at the end of 2012 a solution was proposed that is
(1) compatible with the receiver cabin and future
instruments constraints, (2) preserves the solution
of a mechanical Nasmyth system, (3) preserves the
possibility of a future 2 axis motorization, and (4)
free even more spacing than the current smaller
FOV system. This solution is currently studied by
the Granada team to define its feasibility (structure
stiffness, vibration and thermal characteristics, etc.).
Annual report 2012
37
SIS GROUP
During the year 2012 junction fabrication in the IRAM
SIS group has progressed with high pace to be ready
for the EMIR upgrades and the NOEMA receivers.
Work has focused on new 100 GHz and 150 GHz
wideband mixer designs. Other production runs were
also performed for modified wideband designs for
the 350 GHz band of the SMA.
In the area of kinetic inductance detectors (KIDs),
the development of TiN films has gained in quality
when the specific sputter equipment was upgraded
with a modern mass spectrometer which can work
as well as in pre-process UHV conditions as well
as during reactive sputtering. At the current stage
the pre-sputter conditions could be significantly
improved and stabilized, a very difficult but essential
task if Ti is deposited due to its high reactivity with
background pollutions such as oxygen and water.
Progress has also been made in the characterization
of deposited TiN films by means of X-Ray diffraction
and spectroscopic ellipsometry. For the fabrication
of 4” KID detector arrays such as foreseen for the
NIKA 2 project on the 30m telescope, the SIS group
has upgraded its photolithography line. The work
for KID detectors has received support from the
French LABEX excellence program FOCUS (PI IPAG
Grenoble). The structure of KID arrays as developed
in the NEEL/IRAM collaboration is employing long
CPW readout lines across the array. Such transmission
lines are sensitive to develop undesired asymmetric
modes of propagation. Air-bridges to suppress such
modes have been started to be developed in 2012
an activity which bases on the process previously
developed for cryogenic MEMS applications.
The deposition of membranes, their release and
structuring have made important progress in 2012
and the technology blocks for creating complex fully
planar membrane supported mm-wave structures
have now been assembled. A first application is
underway within the collaboration with INAF to
fabricate a planar wide band OMT for the 100 GHz
range.
BACKEND GROUP
THE HIGH-SPEED ADCS FOR THE NOEMA CORRELATOR ARE IN HOUSE
After a technical evaluation period in close
collaboration with the E 2V-Grenoble chip designers,
it was found that using the EVX 5AS 210 in two-core
mode was a perfectly adequate solution for the
PolyFiX correlator design. A probable weakness in
the clock tree feeding the two other cores make
them less stable, thus not recommended for radio
astronomy. However, as a demonstrator, a 4-core, full
speed (16Gsps) machine was implemented in the
lab and did provide nice single-chunk 8GHz spectra.
The PolyFiX application will be less stringent (2-core
mode) thus will yield superior performance.
This prototype chip is not commercialized by E2V
but 120 pcs have been encapsulated from an existing
batch. All of them were individually tested, showing
an ENOB better than 4.3 bits on the 2 healthy cores.
Prototype of a membrane
based planar orthomode
transducer using a sputtered
SiN membrane on high
resistivity Silicon substrate
and Nb films for the
definition of the waveguide
probes.
38
DEVELOPMENT OF CORRELATOR
The digital “LO 3” phase rotators have been designed,
simulated and aggregated to the Polyphase Filter
Bank on the DiFER platform. Actually the phase
shift is not applied on a physical LO 3 but on the
baseband signal produced by the PFB. Each digital
stream is multiplied by a unity gain complex number
that changes with time at a programmable rate.
Multiplications are performed in I-Q multipliers made
out of DSP blocks from the FPGA. The 16-bit design
allows for a 2.46 km maximum baseline and has
negligible AM and PM residual modulation.
Filters for the IF processor diplexer have been
selected, and two full signal chains prototyped,
including their home made synthesized LO’s. Phase
stability and noise were found very good.
LO REFERENCE SYSTEM FOR 12 ANTENNAS
The design is completed and most components
have been delivered. Several signal chains have been
prototyped in order to measure phase stability and
cross-talk between antennas. The results are an order
of magnitude better than the existing system, due
to modern electronics. The computer-closed loop
is now implemented in a single PC, yielding a faster
transient response.
MECHANICAL GROUP
MICROWAVE DRAWING OFFICE AND MECHANICAL WORKSHOP
The IRAM microwave drawing office worked on
numerous mechanical designs in close collaboration
with the other groups. 80 % of its activities have
Cold NOEMA optics machined
in the IRAM workshop.
been dedicated to NOEMA projects. Other work is
related to the NIKA project and the prototyping of
components for future multibeam systems.
For the NOEMA project, the drawing office and
the IRAM mechanical workshop mainly worked on
specific improvements of the antenna design, on the
prototyping of new receiver components and on
the definition of technical specifications in order to
optimize component assembly.
The workshop did produce a large number of
microwave components, like mixers, couplers, horns
and mirrors. 90 % of the parts dedicated to the
NOEMA project have been produced in the IRAM
workshop.
WORK FOR THE NOEMA PROJECT
The drawing office worked on many mechanical subprojects related to improvements of the current PdB
antenna for NOEMA. Some of them are described
hereafter:
Reflector mass The mass of the reflector is
an important parameter of the telescope as it
determines not only gravitational deformations
but also the lowest eigen-frequency and therefore
the quality of telescope tracking. Right from the
beginning of the NOEMA project, it has been
decided to make a dedicated effort on reflector
weight reduction and work has focused on the
following points:
Backstructure Nodes The weight of the nodes
close to the panels is 6,2 kg. As there are more than
150 such nodes in the reflector and considering
the required counterweights, a mass reduction of
the individual nodes has an important impact on
the total weight of the reflector. After extensive
engineering studies, IRAM succeeded to design a
modified node with 20% weight reduction. This
generates about 500kg of reflector mass reduction.
Annual report 2012
39
Left: Current node.
Right: New node with 20 %
mass reduction
At the time being, prototyping for extensive testing
of the new nodes is engaged, and if successful,
production of the nodes for the first antenna of
NOEMA will be started right after.
Panel actuators The current mass of actuator
is about 500 gr. With our supplier we succeeded
to reduce mass by a factor of 1.5. This concept
generates a total mass reduction for the reflector of
250 kg.
Drawing of the new type of
actuator
DESIGN OF NEW SUBREFLECTOR BACKUP STRUCTURE
One of the main objectives within the antenna
development program for NOEMA is to optimize the
back up structure of the subreflector. The new SRBUS must reach the following main goals:
Improve reliability
Stay with the same mechanical specifications or
better
■■ No extra weight,
■■ Easy maintenance
■■ Limited development and budget risk
■■ Can be directly integrated in the existing PdB
antennas for future upgrades.
■■
■■
Along these lines and in collaboration with SYMETRIE
(Nîmes) IRAM has designed a specific hexapod
device. The mains characteristics of this hexapod are
its possibility for full steering, its carbon fiber based
platform and the improved thermal design of the
support-mirror ensemble.
Previous connections between support and mirror
were made through 4 asymmetrical points; The new
hexapod is designed to have 3 symmetrical points
with a connection with a specific thermo-mechanical
decoupling devices made from INVAR. The
improvement on deformations under thermal stress
is significant and can be seen in the figure below.
3-D view of NOEMA
subreflector mirror with its
hexapod support
All components of the NOEMA subreflector hexapod
have been designed following the very demanding
specifications on environmental conditions at
Plateau de Bure and for the composite parts within
the system special rapid ageing tests are made for
validation.
FEM modeling of deformation
under thermal stress: actual
PdB subreflector (left), and the
NOEMA subreflector (right).
40
PREPARATION AND CONSTRUCTION START OF ANTENNA 7
Year 2012 has been crucial to prepare our technical
team for on site assembling of the NOEMA antennas.
A full work break down, from subcomponent
acceptance over transport and assembling until
final integration and tests, has been established. A
full day-to-day planning has been defined together
with the personal at Plateau de Bure. A matrix
organization involving staff from several groups
and well defined responsibilities will be applied and
operational planning tools have been created.
Machining and factory
pre-assembling of the first
NOEMA antenna mount.
Annual report 2012
COMPUTER GROUP
2012 was a pivotal year for the computer group
because a quick sequence of leaving for retirement
has juxtaposed on the NOEMA project. Fortunately,
after some unavoidable delays, a new group leader
has finally been appointed and the staff has been
reconstituted.
NETWORK INFRASTRUCTURE
In 2011, the headquarter routers have been replaced
by Linux computers. In 2012 the Plateau de Bure
routers have received the same treatment. In parallel
a new SDSL network link has been subscribed to
connect both sites through two different paths.
With such Linux routers at both ends, links can be
aggregated to a single IP tunnel. The new system
offers redundancy and a bigger bandwidth, and it is
totally transparent for the users and applications.
Massive fiber optic deployment is now a national
goal for the French government, therefore new
contacts have been started again with France
Telecom and the local authorities to benefit from a
high-speed network connection at Bure.
HARDWARE AND SOFTWARE UPGRADE
Following the NOEMA project, more powerful
computers are required to run the last-generation
CAD tools in all the technical groups. Therefore a
large program has been launched to upgrade the
computers. Windows 8 has not been considered
as mature enough for IRAM needs, therefore this
upgrade program is based on new DELL workstations
running Windows 7 64 bits. Unlike Windows 8,
Windows 7 requires a very limited training effort for
users because almost all of them already use it at
home for their personal computers.
NOEMA SUPPORT
The computer group was heavily involved in many
work packages for the NOEMA project. For example
it has modified control software to allow the future
double array mode and it has also delivered new
control boxes for the new YIG local oscillator.
ANTENNA CONTROL
A mechanical analog for the new antenna drive
system has been built to test all the new control for
the NOEMA antenna. After that, a scale test with the
new selected motors has been run in September
2012 on antenna #5. The test has shown that these
new motors suit IRAM needs.
Thanks to the drove anolog, the computer group has
also gained a strong experience with EtherCAT on
realtime Linux. This precious knowledge will be used
to develop the final antenna control software.
41
42
SCIENCE SOFTWARE ACTIVITIES
The main goal of the science software activities at
IRAM is to support the preparation, the acquisition
and the reduction of data at both the 30m and
the Plateau de Bure Interferometer. This includes
the delivery of 1) software to the community for
proposing and setting-up observations, 2) software
to the IRAM staff for use in the online acquisition
system and 3) offline software to end users for final
reduction of their data. However, the GILDAS suite
of software is freely available to and used by other
radio telescopes, like Herschel/HIFI, APEX and SOFIA/
GREAT.
At the 30m, the advent of broadband spectra (16
GHz per polarization) at high spectral resolution
(195 kHz) triggered in 2010 a series of changes in
the data processing and analysis of spectra. Many
adaptations of the data processing software (CLASS)
were finalized in 2012. This includes generalizations
in the handling of the spectroscopic axes to remove
assumptions valid only for narrow-band spectra.
In addition, adaptations were made to take into
account the evolution with frequency of telescope
parameters, like the beam efficiencies. Moreover,
the associated increase of the data rate underlined
efficiency problems in MIRA, the online calibration
software. In view of the difficulty to solve them, it
was decided to develop a new efficient and robust
calibration software. A first version of this software,
named MRTCAL, should be available end of 2013 or
beginning of 2014. The interface to line databases
(CDMS, JPL, etc.), developed in 2010 in collaboration
with the Observatoire de Grenoble, and released
as a CLASS extension named WEEDS, proved its
usefulness. A new round of developments thus
started in 2012 to generalize this service and to make
it available to other GILDAS software. The monitoring
of the technical properties (time synchronization,
tracking, pointing, focus, calibration, etc.) of the 30m
continued. For instance, statistical analyses were
developed in MOPSIC to reveal and to understand
systematic behaviors. Work started to use the same
tools for the Plateau de Bure interferometer.
After a round of software requirements for NOEMA,
the Plateau de Bure interferometer extension
project, the first developments happened in 2012.
At this early time in the project, work focused on
preparation. Three main actions happened on
the data acquisition side. First, the possibility to
separate the array of antenna into two sub-arrays
was introduced. This will be essential to enable
simultaneously science observations along with
commissioning phases of new hardware (antenna,
receivers, correlators, etc.) from 2014 to 2017. This
implied significant changes in the real-time software
to be able to separately control some pieces of
hardware from both arrays and to synchronize the
access to shared resources (e.g. the noise diodes
used for calibration). Second, prototype hardware,
like a new tiltmeter, was integrated into one of
the existing PdBI antenna, implying new software
to command them, store the measurements, and
analyze the results. Third, a general review of the
codes developed in the last five years happened
to base further developments on firm grounds.
This includes removal of obsolete commands,
debugging, and improvements in the handling
of the backward compatibility over the last few
generations of receivers. As a consequence, the
software that interfaces the online acquisition of the
array (OBS) can now be started without hardware
resources, a first step towards the implementation of
a simulator mode.
Support for science operations continued in 2012.
Many improvements were implemented in the
calibration pipeline: 1) Efforts were done to identify
parasites into the radio-frequency passband; 2) The
size of the secondary flux calibrator (MWC349) was
taken into account in the flux calibration, as this
source starts to be resolved in the A-configuration;
3) A new tool was included to assess whether a
faint line is detected inside the receiver bandpass.
This is particularly useful to detect galaxies at
high redshift. The calibration pipeline is now fully
mature, i.e. it provides optimized solutions for all
calibration steps, except the flux calibration – work is
progressing to bring it to the same level of maturity.
Moreover, a tool intended to aid astronomers on
duty and operators in optimizing the interferometer’s
observing schedule on a 24 hours timescale is being
developed in collaboration with the Observatoire de
Grenoble.
The size of the datasets produced by the current and
future radio-instruments experience a tremendous
increase (because of the multi-beam receivers, wide
bandwidth receivers, spectrometers with thousands
of channels, and/or new observing modes like the
interferometric on-the-fly). This implied a transversal
work to remove the limitations present in all the data
formats used in GILDAS. We first concentrated on the
GILDAS Data Format (GDF) to store already calibrated
data, either position, frequency cubes or calibrated
uv-tables. This project (known as GDF-V 2), which
was started in 2011, aims at enabling the support of
arrays of more than 2 giga elements (the limit that
a 32 bits integer can encode). This has implications
on all GILDAS software. This change is done so
that GILDAS will still be able to read the version 1
of the format to ensure backward compatibility
Annual report 2012
with existing data sets. The project will converge
in 2013. This work is done in collaboration with the
Observatoire de Bordeaux. Additionally, we worked
on the data formats to store raw data both from
the IRAM-30m and the PdBI, i.e. the CLASS and
CLIC data format, respectively. While the semantics
(i.e. the meaning) of both data format are very
different due to the specificities of the single-dish
and interferometry techniques, CLASS and CLIC still
share the data binary container (i.e. the way the bits
are ordered, independent of their science meaning).
After an analysis of the different limitations of this
data binary container, we progressively removed
them. In order to factorize the code, we created
a new library, named CLASSIC, which will be
used in both CLASS and CLIC. This will decrease
maintenance efforts on the medium term.
All the software developments are based on the
common GILDAS services, e.g. a set of common
low-level libraries, collectively named GILDAS
kernel, which take care of the scripting and
plotting capabilities of GILDAS. Among the many
small improvements which happened in 2012, a
particular effort was done to improve the new users’
learning curve: the various help documents and
demonstration scripts were made easily available
inside the main widgets of the different programs.
We also ensured that GILDAS is able to import/
export the FITS format of the CASA software
developed for ALMA and the eVLA. Finally, the PMS
(Proposal Management System) project, which
will replace the current proposal submission and
processing system for the IRAM 30m telescope and
Plateau de Bure interferometer, was successfully
used during the process of the proposal technical
evaluation and during the two program committee
meetings in 2012. Work started on the new proposal
submission facility, which will first be used in
September 2013.
43
Credit: ALMA (ESO/NAOJ/NRAO)
44
IRAM ARC Node
The IRAM astronomy support group has been
involved for many years in several ALMA-related
activities and software developments, hence
building an important expertise in the ALMA
instrument. IRAM is now a node of the European
ALMA Regional Center (ARC) and provides direct
support to ALMA users. On the long term, having
access to NOEMA and to the ARC node services
should place the IRAM users community in the best
possible position to obtain observing time on ALMA,
in an extremely competitive environment.
TELESCOPE CALIBRATION SOFTWARE
IRAM is responsible for the development and
maintenance of one of the key software for the realtime operations of ALMA, the Telescope Calibration
(TelCal) software. An amendment to the original
agreement between ESO and IRAM was signed in
2012 to extend and increase the IRAM contribution
for TelCal in 2013 and 2014. TelCal is performing all
real-time calibrations necessary to run the array:
antenna pointing, focus, baseline measurements,
atmospheric parameters, etc. Two IRAM engineers
are working on these developments.
software was used all over the year to perform
scientific observations (Cycle 0), putting strong
constraints on the performances and reliability of the
real-time system. In parallel, the array commissioning
continued, implying a continuous and important
effort to correct, adapt, and further develop TelCal.
A stand-alone version of TelCal, interfaced to the
CASA off-line package, is also supported, to allow
an off-line reprocessing of the real-time calibration.
Finally, a specific version of CLIC, used for the ALMA
holography processing, is also maintained in the
TelCal package.
2012 was a critical year for TelCal, as this was the
first year during which a production version of the
ALMA USERS SUPPORT
2012 was a pivotal year for the ARC, as the start of
the scientific operations (end of 2011) triggered an
important series of activities. The main tasks the IRAM
ARC node was involved in were:
■■
Preparation of the Cycle 1 deadline; various
documents were distributed in order to help the
IRAM community to prepare their proposals.
■■
Cycle 0 contact scientists: the ARC node staff act
as “Contact Scientists” for the accepted ALMA
projects, providing expertise to check and validate
the Scheduling Blocks that were created from the
initial proposals. The IRAM ARC node supported
20 projects out of the 54 accepted+filler projects
in Europe. Specific tools to display and possibly
Annual report 2012
optimize the correlator setup in the ASTRO
software were developed.
■■ Face-to-face support for data reduction: from July
2012 on, IRAM started to support astronomers
visiting the institute for the reduction of their
ALMA projects. Procedures similar to the Plateau
de Bure rules were used to organize these visits,
including financial support for PIs affiliated to the
45
IRAM funding agencies. The data reduction itself
turned out to be a somewhat lengthy process,
as many calibration parameters have still to be
manually checked and optimized, providing in
some cases a significant increase of the final maps
quality. Data fillers to transfer calibrated data from/
to CASA to/from GILDAS were developed, allowing
to image the data in both software packages.
8TH MM INTERFEROMETRY SCHOOL
IRAM organized its 8th mm-interferometry school
from October 15-19, in Grenoble. The lectures
covered, as in the previous schools, the fundamentals
of millimeter interferometry techniques, the
atmospheric phase correction, data calibration,
and imaging. The Plateau de Bure array and ALMA
were presented in some details, and data reduction
tutorials were also organized. 65 participants - out
of more than 120 applications - attended the school
and gave a very positive feedback at the end of the
week. This event was supported, as in 2010, by the
EU RadioNet program.
Participants at the 8th IRAM
interferometry school
46
Personnel and finances
HUMAN RESOURCES
In 2012, IRAM employed 93 FTE in France and 29.5
FTE in Spain.
Five employees joined IRAM in 2012:
Grégoire Coiffard (PhD-student), Xavier Avrillier,
Sabine König and Tessel Van der Laan to reinforce
the scientific and technical departments; Isabelle
Delaunay in the administration department.
Six employees left IRAM at the same time:
Irvin Stil, Roger Ah Tchou, Markus Rösch (PhDstudent), Mathieu Lonjaret and Jean Yves Pierre from
the scientific and technical departments ; Raymond
Hennequin from the administration department.
IRAM gratefully thanks these persons for their work
and involvement through years. IRAM also thanks
Martino Calvo (now Inst. Neel) who strengthened the
IRAM NIKA team for six months in 2012.
On the whole 34 employees were assigned to
science tasks and 82 to technical or administrative
positions. IRAM science staff is concerned with the
operation of the observatories and the science
support of IRAM users. The technical departments
of IRAM are in charge of design, production and
maintenance of IRAM’s equipments. With their work
they provide the international scientific community
with one of the world finest equipments in the field
of millimetre astronomy. The IRAM Administrative
staff allows IRAM to find its way through the
increasing complexity of national and iternational
administrative tasks.
The performance of IRAM’s personel is also the result
of the high level of qualification and involvement of
IRAM staff. To support this, IRAM has carried out an
important training policy for years and will continue
to do so.
Annual report 2012
IRAM is also a women-friendly institute, 30% of
IRAM employees are women, a percentage which is
independent of qualification level.
OPERATING AND INVESTMENT BUDGETS - 2012
The IRAM associates approved a 2% increase in
their base contribution to the operation budget for
2012. The contributions to the investment budget
were maintained at their previous level for 2012.
In addition, CNRS transferred for 2012 a specific
contribution of 1 M€ to the investment budget as
Expenditure
Income
Budget heading
Approved
Actual
Operation/Personnel
8 216 493
8 148 292
Operation/Other items
3 329 937
421 143
11 967 573
11 497 703
1 565 816
818 781
Investment NOEMA
9 595 267
1 933 043
Investment Cable Car
9 384 474
210 891
Budgetary excess/loss
TOTAL OPERATION
Investment base
Budgetay excess/loss
TOTAL EXPENDITURE excl. VAT
part of the participation in the reconstruction of the
cable car to access the Plateau de Bure Observatory.
Finally, 6,5 M€ were budgeted and transferred by
ANR (Agence Nationale de la Recherche)-EQUIPEX to
co-finance the NOEMA Phase 1.
Budget heading
Approved
Actual
CNRS contributions
7 276 589
7 276 589
3 683 725
MPG contributions
5 776 589
5 776 589
-334 315
IGN contributions
17 896 315
32 513 131
32 356 733
TOTAL CONTRIBUTION
Carry forward from previous years
737 437
737 437
13 790 614
13 790 614
6 202 287
6 202 287
IRAM’own income
6 020 230
5 863 832
ANR EQUIPEX
6 500 000
6 500 000
32 513 131
32 356 733
TOTAL INCOME excl. VAT
47
Annual report 2012
49
Annex I – Telescope schedules
The next two tables show the allocations for the telescope time for the 30-meter telescope and the Plateau de Bure Interferometer for the
year 2012. In each table, the first column gives the project’s identification, the second column the title of the investigation and the third
column the names of the Principal Investigators and the co-investigators.
30-METER TELESCOPE
Ident.
Title
Investigators
228-09
A Legacy Survey to Study Cold Gas Scaling Laws in the
Local Universe
Kramer, Kauffmann, Buchbender, Catinella, Cortese, Fabello, Fu, Giovanelli, Gracia-Carpio, Guo, Haynes,
Heckman, Krumholz, Li, Moran, Rodriguez-Fernandez, Saintonge, Schiminovich, Schuster, Sievers,
Tacconi, Wang
225-10
The complete CO(2-1) map of M33
Braine, Schuster, Kramer, Gonzalez, Sievers, Rodriguez, Gratier, Brouillet, Herpin, Bontemps, Israel, van
der Werf, van der Tak, Tabatabaei, Henkel, Roellig, Combes, Wiedner
271-10
Physics of Gas and Star Formation in Galaxies at z=1.2
Combes, Tacconi, Genzel, Bolatto, Bournaud, Burkert, Cooper, Cox, Davis, Schreiber, García-Burillo,
Gracia-Carpio, Lutz, Naab, Neri, Newman, Sternberg, Weiner
135-11
Isotopic ratios in Oort cloud comet C/2009P1 (Garradd) Biver, Bockelée-Morvan, Crovisier, Colom, Moreno, Hartogh, Lis, Boissier, Paubert, Weaver, Russo, Vervack
136-11
Search for complex organic molecules in pre-stellar
cores
Bacmann, Kahane, Taquet, Ceccarelli, Faure
137-11
Using chemistry to constrain the evolutionary state of
prestellar cores
Maret, Tafalla, Bergin, Hily-Blant
138-11
A search for formamide in the solar-type protostar IRAS
16293-2422
Kahane, Alexandre, Alexandre, Cecilia, Vianney, Laurent, Roman, Eric
139-11
Chemical characterisation of the massive cores in IRDC
G28.53-00.25
Padovani, Girart, Palau, Sepulcre, Busquet, Sánchez-Monge, Frau
140-11
The chemical structure of Orion : Completion of the 2-D Marcelino, Cernicharo, Esplugues, Palau, Bell, Tercero, Guelin
line survey at 1mm
142-11
Search for ortho-H2Cl+, a new probe of the diffuse ISM
Gerin, Neufeld, De Luca, Kramer, Le Petit, Lis, Menten, Navarro, Pety, Roueff
143-11
Spectroscopy of Shocks: the role of SiO(8-7)
Codella, Gueth, Cabrit, Ceccarelli, Lefloch, Bachiller, Tafalla, Guilloteau, Benedettini, Gusdorf, Nisini
145-11
Benchmarking grain-surface chemistry on the
Horsehead mane
Pety, Guzman, Bardeau, Belloche, Gerin, Goicoechea, Gratier, Le Bourlot, Le Petit, Roueff, Teyssier, Sievers
146-11
Search for 13C Ethanol toward G34.3 +0.15, a star
forming region
Bouchez Giret, Bottinelli, Walters, Müller
149-11
Deuterated water chemistry towards high/low-mass
star-forming regions.
Vastel, Gérin, Coutens, Comito, Jastrzebska, Lis, Goldsmith, Herbst, Faure
150-11
D3O+ and the oxygen budget of L1544
Bizzocchi, Caselli, Dore, Ceccarelli, van der Tak, Angeloni, Leonardo
152-11
Deuterium fractionation in the evolution of high-mass
protostars
Fontani, Sánchez-Monge, López-Sepulcre, Cesaroni, Walmsley, Beltrán
153-11
Search for deuterated methyl formate (DCOOCH3) in
NGC1333-IRAS4A
Demyk, Bottinelli, Caux, Vastel, Coutens, Ceccarelli, Kahane, Taquet, Wakelam, Quirico, Ratajczak, Aikawa
154-11
Isotopic fractionation of nitrogen in the dense and
cold ISM.
Le Gal, Hily-Blant, Padovani, Faure, Pineau des Forêts, Walmsley, Tafalla
155-11
A 1 mm high spectral resolution line survey of the
Orion Bar PDR
Goicoechea, Cuadrado, Cernicharo, Fuente, Esplugues, García-Burillo, Usero, Marcelino
156-11
An Unbiased Spectral Survey of the Protostellar
Bowshock L1157-B1
Lefloch, Ceccarelli, Gueth, Cernicharo, Codella, Benedettini, Cabrit, Schuster, Vasta
157-11
Spectral survey of the intermediate mass protostar
OMC2-FIR4
López-Sepulcre, Kama, Ceccarelli, Lefloch, Fuente, Caselli, Caux, Dominik, Kahane, van der Tak,
Wiesenfeld
158-11
A complete 3mm line survey of dark cloud cores: B1-b
and TMC-1
Marcelino, Cernicharo, Roueff, Thum, Gerin
159-11
Molecular study of the PDR around the UCHII region
Mon R2
Treviño-Morales, Fuente, Kramer, Gonzalez-Garcia, Pilleri, Cernicharo, Ginard, Berne, Joblin, Ossenkopf,
Goicoechea, Garcia-Burillo, Roueff, Viti, Rizzo, Alonso-Albi
161-11
Unbiased Line Spectral Survey of a Circumstellar Disk
Hily-Blant, Kastner, Forveille, Sacco, Rodriguez, Zuckerman
162-11
Probing the magnetic field in Supernova Remnant IC
443
Hezareh, Wiesemeyer, Gusdorf, Thum
163-11
Preliminary Observations for a Large Zeeman Proposal
Falgarone, Crutcher, Troland, Hily-Blant, Piétu, Paubert, Guilloteau, Beuther, Heiles, Lai, Koch, Tang,
Zhang, Henning, Plambeck
164-11
3D magnetic fields and deep chemical survey of young Frau, Padovani, Girart, Beltrán, Morata, Alves, Franco
magnetized prestellar cores
165-11
Magnetic Fields versus Turbulence on Regulating Star
Formation
Li, Kainulainen, Houde, Henning
50
Ident.
Title
Investigators
167-11
IRAM-30m follow-up of cold cores detected by the
Planck satellite
Pagani, Ristorcelli, Juvela, Bernard, Giard, Mény, Marshall, Montier, Harju, Malinen, Laureijs, Mcgehee,
Paladini, Pelkonen, Toth
169-11
Understanding core formation in clustered
environments
Hacar, Tafalla
170-11
New it Herschel-identified Orion protostars:
characterizing an extreme population of cold sources
with IRAM
Stutz, Tobin, Thomas Megeath, di Francesco, Henning, Linz, Stanke, Ali, Fischer, Maret, Wilson
171-11
Outflow Impacts on the Protocluster Serpens South
Plunkett, Arce, Mardones, Chen, Dunham
172-11
Carbon budget and molecular cloud formation
signatures in IRDCs
Ragan, Beuther, Linz, Henning
173-11
Interaction of cosmic-rays and molecular clouds
Ceccarelli, Dubus, Hily-Blant, Lelfoch, Montmerle, Padovani
174-11
Tracing infall towards the low-luminosity protostar in
CB130
Lippok, Launhardt, Stutz, Henning, Linz, Pavlyuchenkov, Semenov
175-11
Rotation Signatures in the Inner Protostellar Envelope:
Constraining Angular Momentum
Tobin, Bourke, Stutz, Smith, Wootten, Maret, Bergin, Hartmann
176-11
The outflow phenomenon at the substellar boundary
Monin, Lefloch, Dougados, Whelan, Cabrit, Oliveira
177-11
Origin of warm water in deeply embedded low-mass
protostars
Persson, Jorgensen, Dishoeck, Harsono, Visser, Kristensen, Bergin
178-11
MAYS: Mass (and ages) of Young Stars - a CN survey
Guilloteau, Di Folco, Simon, Piétu, Dutrey, Hersant, Wakelam, Ducourant, Grosso, Guillout, Schaefer,
White, Teixera, Palla
179-11
Structure and Kinematics of Hub-Filament Systems in
High-Mass Star Formation
Liu, Quintana-Lacaci, Immer, Menten, Wang, Ho, Zhang, Galván-Madrid, Lin, Li, Zhang
180-11
The systematic trends in the kinematics of massive star
forming regions. Observations of HC3N* in hot cores
Rivilla, Martín-Pintado, Jiménez-Serra, Rodríguez-franco, Báez
181-11
The evolution of outflows in high-mass young stellar
objects
Sánchez-Monge, López-Sepulcre, Cesaroni, Walmsley, Codella, Beltrán
182-11
Probing the large scale chemical evolution in highmass protostars
Øberg, Fayolle, Dishoeck, Garrod, Bisschop
183-11
Mass loss on the RGB: reaching the limits
Groenewegen
184-11
Studying the outer molecular envelope of Betelgeuse
Kamiński, Proedrou, Menten
185-11
Search for rotating disks around Hot post-AGB stars.
Quintana-Lacaci, Akras
186-11
Mass-loss properties of AGB stars: the key to
understanding wind-ISM interactions
Cox, Groenewegen, Decin, Royer, De Beck
187-11
Discs around post-AGB stars and the formation of
planetary nebulae
Bujarrabal, Winckel, Alcolea, Santander-García, Castro-Carrizo
188-11
A Line Survey of the Supergiant O-rich star VY CMa
Cernicharo, Quintana-Lacaci, Sánchez Contreras, Velilla, Bujarrabal, Marcelino, Alcolea, Santander,
Pearson, Teyssier
190-11
2 mm Continuum Observations of the Galactic Center
Region
Staguhn, Kovács, Benford, Morris
191-11
The accretion flow onto Sgr Astar
Thum, Downes, Morris, Sievers, Wiesemeyer
193-11
EMIR CO and CO maps of the M83 central bar
(resubmission)
Abreu Vicente, Kramer, García-Burillo, Israel, Lord, Billot
195-11
Molecular gas mass distribution in NGC 604 (M 33)
Israel, Braine, Heiner
196-11
CO in Abell 1367: a probe for interaction mechanisms
Scott, Brinks, Usero, Bravo-Alfaro
197-11
CO Gas Clouds toward the Virgo Cluster: Progenitors of
Dwarf Galaxies
Kent, Mangum
199-11
A Unique Dynamical Measurement of Star-Formation
Thresholds in Five Galaxy Disks
Westfall, Verheijen, Spaans, van der Tak, Bershady, Martinsson, Kramer
200-11
The Physical State of Dense Molecular Gas in Early-Type Crocker, Bournaud, Juneau, Saintonge, Martig, Bureau
Galaxies
201-11
Monitoring the HNC/HCN ratio in Arp220
Aalto, Costagliola, Muller, Martín, Sakamoto, Garcia-Burillo, Cernicharo
203-11
Constraining the origin of the heating rate in the
Perseus Cluster
Bayet, Viti, Hartquist, Williams, Aladro
204-11
Characterisation of the very dense gas in the outskirts
of NGC6946
Bayet, Viti, Martín-Pintado, Martín, Aladro
208-11
Exploring Averaged Chemical Composition of GMCs in
the Spiral Arm of M51
Yoshimasa, Sorai, Sakai, Yamamoto
209-11
Cold dust along the major axis of the spiral galaxy M33
- the HerM33es project.
Quintana-Lacaci, Kramer, Sievers, Bertoldi, Albrecht, Buchbender, Tabatabaei, Akras, Xilouris, Alto,
Anderl, Braine, Israel
210-11
Molecular shocks in the Stephan’s Quintet
Usero, García-Burillo, Verdes-Montenegro, Fuente, Sulentic, Brinks
211-11
Dense gas tracing the collisional past of Andromeda: an Melchior, Combes
atypical inner region?
214-11
Molecular content of polar ring galaxies
12
13
Combes, Reshetnikov, Moiseev
Annual report 2012
51
Ident.
Title
Investigators
216-11
Molecular gas masses for a sample of local mergers:
bridging the gap between normal galaxies and ULIRGs
in the Kennicutt-Schmidt law
Coppin, Scudder, Ellison
218-11
Using IRAM to Construct the First Detailed Timeline of
Early Type Galaxy Evolution
Zabludoff, Shirley, Yang, Walter, Narayanan, Smith
219-11
Star Formation in Void Galaxies
Beygu, Van Der Hulst, Van De Weijgaert, Gorkom, Kreckel
220-11
Dust and molecular gas in Virgo star-forming dwarf
galaxies
Grossi, Corbelli, Hunt, Bianchi, Giovanardi, Magrini, Pappalardo, Madden, Davies, Smith, Bizzocchi,
Papaderos, De Looze, Verstappen, Garcia, Vlahakis
221-11
Mapping the molecular inner ring of M31
Melchior, Combes
222-11
CO properties of the most gas-rich massive galaxies up
to z~0.2
Cortese, Catinella, Fabello
223-11
Are mid-IR spectral signatures of pressure-confined
star formation an aspect of major merger mode star
formation in galaxies?
Spoon, Aalto, Costagliola, Farrah, Garcia-Burillo, Illana, Graciá-Carpio, Lahuis, Pérez-Beaupuits, PerezTorres, Rodriguez, Spaans
224-11
Molecular Tracers of Galaxy Evolution II: Chemistry or
Excitation?
Costagliola, Aalto, Spoon, van der Werf, Muller, Jütte, Lahuis, Martín Ruiz, Rodriguez
225-11
CS 2-1/3-2 mapping along the major axes of nearby
gas-rich galaxies
Zhang, Henkel, Gao, Wang, Garcia-Burillo, Graciá-Carpio
226-11
The nuclear ISM of Luminous IR Galaxies
Baan, Henkel, Papadopoulos, Loenen, Meijerink
227-11
Molecular Gas Observations of LIR ≥ 1011.4 Lx Infrared
Galaxies in the Great Observatories All-sky LIRG Survey
(GOALS)
Iwasawa, Evans, Aalto, Frayer, Perez-Torres, Herrero-Illana, Surace, Privon, Kim, Mazzarella, Armus, Spoon
229-11
Probing the kinetic temperature in active galaxies
Rodríguez, Mühle, Aalto, Odriozola, Pérez Torres
230-11
Characterising the influence of galaxy activity on the
properties of the densest molecular gas component
231-11
Multi-line HCO+ survey in external galaxies - Part I.
Starburst
232-11
The physical conditions of molecular gas in extreme
star-forming environments
Davis, Heiderman, Iono, Blanc, Evans, Gebhardt, Papovich, Yun
233-11
Measuring the intrinsic radio power of AGN in cluster
cores with GISMO
Edge, Hogan, Staguhn, Kovács, Benford, Hlavacek-Larrondo, Fabian, Salomé, Grainge
234-11
Searching for SiO mega-maser in type II AGN
Wang, Zhang
235-11
The dense gas properties in the AGN with the most
turbulent H2 gas motions
Dasyra, Combes
236-11
MAPI: Monitoring AGN with Polarimetry at the IRAM-30 Agudo, Thum, Wiesemeyer, Gómez, Casadio, Molina, Marscher, Jorstad
m
237-11
Testing the link between star formation and AGN
Dicken, Nesvadba, Boulanger, Lehnert, Combes, Tadhunter
238-11
Coordinated cm to mm-monitoring of variability and
spectral shape evolution of a selected Fermi blazar
sample
Fuhrmann, Zensus, Nestoras, Krichbaum, Angelakis, Schmidt, Ungerechts, Sievers, Readhead
239-11
A systematic search for absorption lines in z~2 radio
galaxies
Nesvadba, Combes, Garcia-Burillo, De Breuck, Collet, Boulanger, Lehnert, Papadopoulos
240-11
Molecular gas content in radio galaxies at medium
redshift (0.3 - 0.6)
Ocaña Flaquer, Leon, Verdes-Montenegro, Scott
241-11
The molecular gas content of 0.2 < z <0.3 SDSS type 2
quasars.
Villar Martín, De Breuck, Colina, Emonts, Humphrey, Martínez-Sansigre, Pérez-Torres, Rodríguez
242-11
Interstellar Medium Physical Conditions in a Normal
Spiral Galaxy at z=1
Richard, Boone, Dessauges, Egami, Rex, Schaerer, Zamojski, Pello, Combes, Blain, Omont, Kneib
243-11
CO Study for Dust-Rich Quasars at z <= 2
Dai, Omont, Bergeron, Willmer, Huang, Rigopoulou, Hatziminaoglou, Perez-Fournon, Elvis, Fazio
244-11
CO and CI in Intermediate Redshift ULIRGs
Boone, Lim, Gerin, Bayet, Papadopoulos, Dasyra, Combes, Trung, Muller
245-11
Disentangling SZ Clusters and Dusty Galaxies
Kovács, Staguhn, Benford
246-11
New strongly lensed galaxies representative of the
high-z star forming population
De Zotti, Maiolino, González-Nuevo, Andreani, Lapi, Danese, Negrello, Dannerbauer, Omont,
Rodighiero, Fan, Serjeant, Birkinshaw, Clements, Smail, Michalowski, Wardlow, Dye
247-11
COSMO: Characterizing the High Redshift Tail of the
SMG Population
Staguhn, Karim, Schinnerer, Smolvcic, Bertoldi, Aravena, Smail, Benford, Kovács
248-11
Millimeter Photometry of FIR-Bright High Redshift WISE Benford, Bridge, Eisenhardt, Petty, Tsai, Wright, Wu, Blain
Sources
249-11
GISMO snapshots: Obtaining the flux at 2 mm of the
Brightest Herschel-Selected Submm-Galaxies at z>5
Perez Fournon, Dannerbauer, Bertoldi, Omont, Riechers, Clements, Conley, Cox, Ivison, Michalowski
250-11
The GDF: The Deepest (Sub-)Millimeter Field Ever
Staguhn, Walter, Kovács, Benford, Decarli, Da Cunha
251-11
Chasing dust in strongly lensed z>6 star-forming
galaxies
Schaerer, Staguhn, Dessauges, Boone, Combes, Kneib, Richard, Zamojski
252-11
High-J CO lines of lensed high-z galaxies discovered by
Herschel
van der Werf, Omont, Ivison, Cox, Swinbank, Smail, Dannerbauer, Bertoldi, Rosenberg, Eales, Cooray,
Leeuw, Ibar, Vaccari, Coppin, Dunlop, De Zotti, Harris, Baker, Verma, Frayer, Meijerink, Loenen, Berciano,
Krips, Lupu, Massardi, Scott, Marrone
52
Ident.
Title
Investigators
253-11
CO Redshift Search for Exceptionally Bright Lensed
Herschel Sources
Kneib, Dessauges-Zavadsky, Boone, Combes, Omont, Egami, Rex, Rawle, Schaerer, Smail, Xu
254-11
Searching for gas in WISE-selected Hyperluminous
Galaxies
Blain, Benford, Bridge, Eisenhardt, Jones, Petty, Yan, Tsai, Wu
255-11
A search for HeH+ at high redshifts
Zinchenko, Dubrovich, Henkel
257-11
The fragmentation of massive dense cores detected
by Herschel
Hennemann, Motte, Csengeri, Schneider, Hill, Luong, Bontemps
260-11
A complete homogeneous CO survey of northern FU
Ori-type objects
Kóspál, Ábrahám, Hogerheijde, Brinch
262-11
Molecular filament in the Crab Nebula
Salomé, Hily-Blant, Castro-Carrizo, Ferland, Combes, Baldwin, Loh, C Fabian
264-11
Dense Gas in M 33 - Complementary 12CO(1-0)
observations
Buchbender, Kramer, Quintana-Lacaci, Gonzalez-Garcia, Garcia-Burillo, Bertoldi, Anderl, Mookerjea,
Braine, Gratier, Billot, Israel
D05-11
CFp as a tracer of Cp, the outermost layers in PDRs
Guzmán, Pety, Gratier, Gerin, Goicoechea, Teyssier, Roueff
D06-11
Isotopic ratios in M82
LeBourlot
D07-11
Extended submillimeter emission in A2744, galaxies
at z>5?
Boone, Schaerer, Lutz, Weiss, Combes, Richard, Dessauges-Zavadsky, Egami, Rex, Rawle, Pello, Staguhn,
Edge, Smail, Ivison, Zamojski, Altieri, Kneib, Omont, van der Werf
D08-11
DDT extension for the complete CO(2-1) map of M33
Braine, Schuster, Kramer, Gonzalez, Sievers, Rodriguez, Gratier, Brouillet, Herpin, Bontemps, Israel, van
der Werf, van der Tak, Tabatabaei, Henkel, Roellig, Combes, Wiedner
002-12
A synoptic view of chemistry in diffuse interstellar gas
Liszt, Pety, Lucas, Gerin
003-12
The puzzling presence of COMs in prestellar cores: role
of photolytic processes
Bacmann, Taquet, Faure, Thiabaud, Quirico, Bonal
004-12
The role of PAH photo-destruction in the carbon
chemistry of PDRs.
Pilleri, Joblin, Berné, Gerin, Montillaud, Fuente, Falgarone, Le Bourlot, Cernicharo, Pety, Kokkin,
Goicoechea, González-García, Treviño-Morales, Kramer, Cuadrado, Godard, Le Petit, Teyssier, Habart
005-12
Deuteration in the PDR around the UCHII region Mon
R2
Treviño-Morales, Fuente, Kramer, Gonzalez-Garcia, Pilleri, Roueff, Gerin, Pety, Cernicharo, Ginard, Berne,
Ossenkopf, Goicoechea, Garcia-Burillo, Viti, Rizzo
008-12
A search for c-C3D2, a new probe for interstellar
deuterium chemistry
Spezzano, Brünken, Schilke, Mccarthy, Caselli
009-12
A Search for Deuterated Ammonium Ion in Molecular
Clouds
Cernicharo, Roueff, Marcelino, Tercero, Fuente, Gerin, Carrasco, Tanarro, Domenech, Herrero
010-12
15
Bizzocchi, Caselli, Leonardo, Dore
011-12
Nitriles in dark clouds: chemistry and isotopic ratios
Bonal, Faure, Hily-Blant, Le Gal, Quirico, Maret, Rist, Padovani, Pineau des Forêts
012-12
IRAM Chemical Survey of Sun-Like Star-Forming
Regions
Bachiller, Lefloch, Cernicharo, Fuente, Tafalla, De Vicente, Alonso-Albi, Rodriguez, Ceccarelli, Kahane,
Bacmann, Hily-Blant, Podio, Le Gall, López-Sepulcre, Faure, Wiesenfeld, Caux, Vastel, Bottinelli, Demyk,
Marcelino, Codella, Vasta, Roueff, Gerin, Pineau Des Forets, Cabrit, Gomez-Ruiz, Viti, Caselli, Sakai,
Yamamoto, Pety, Gonzalez
013-12
Unbiased spectral survey of CygX-N63 a unique pre-hot Bontemps, Csengeri, Fechtenbaum, Herpin, Duarte-Cabral, Hennemann, Schneider, Motte, Gursdorf,
core source
Lefloch, Wakelam
014-12
Building a chemical sequence of starless core evolution: Frau, Girart, Beltrán, Tafalla, Morata, Alves, Franco
a 3mm line survey
015-12
Benchmarking grain-surface chemistry on the
Horsehead mane
Guzmán, Pety, Gratier, Gerin, Goicoechea, Bardeau, Belloche, Le Bourlot, Le Petit, Roueff, Teyssier, Sievers
016-12
An unbiased 3 mm line survey of a protoplanetary disk
Øberg, Graninger, Qi, Wilner
017-12
A Line Survey of the Supergiant O-rich star VY CMa. II
Cernicharo, Quintana-Lacaci, Sánchez Contreras, Velilla, Bujarrabal, Marcelino, Alcolea, Santander,
Pearson, Teyssier
019-12
From Gas Motions to Star-Forming Cores in Perseus
B1-E
Sadavoy, di Francesco, Shirley, André, Hatchell, Pezzuto
020-12
The Stability of Super-Jeans Starless Cores
Schnee, di Francesco, Johnstone, Sadavoy
021-12
Using chemistry to constrain the evolutionary state of
prestellar cores
Maret, Tafalla, Bergin, Hily-Blant
022-12
Probing core growth through filamentary accretion in
Taurus
Palmeirim, André, Didelon, Peretto, Hennebelle, Arzoumanian, Könyves, Menshchikov
024-12
Infall and outflow in young IRDC cores
Ragan, Beuther, Linz, Henning
025-12
Large scale kinematics of the dense gas in IRDCs
Henshaw, Caselli, Tan, Jimenez-Serra, Fontani, Hernandez
027-12
Observations of C O J = 1-0 & 2-1: A Direct Method to
Obtain Total Column Densities in Hot Cores
Plume, Caux, Bergin, Lis, Cernicharo, Menten, Schilke., Stutzki, Wang
028-12
Dust properties in star-forming cores
Launhardt, Stutz, Lippok, Henning, Krause, Nielbock, di Francesco, Staguhn, Kovács
029-12
Understanding the nature of coreshine
Pagani, Andersen, Bacmann, Steinacker
031-12
Short spacing data for SMA observations of S255
Zinchenko, Liu, Su
032-12
Angular Momentum Transportation from Envelopes
to Disks
Yen, Takakuwa, Ohashi, Ho
033-12
The chemical sub-structure of Orion-KL: SMA & 30 m
in concert
Feng, Beuther, Semenov, Henning
N fractionation at the starting point of star formation
18
Annual report 2012
53
Ident.
Title
Investigators
034-12
MAYS: Mass (and ages) of Young Stars - a CN survey in
ρ Oph
White, Teixera, Palla
035-12
A quest for high-mass star formation in two families of
molecular clumps
Cesaroni, Beltrán, Elia, Molinari, Moscadelli, Olmi, Pestalozzi, Sánchez-Monge, Schisano
037-12
Molecular fingerprints of an unbiased sample of
Galactic MSF clumps
Wyrowski, Csengeri, König, Urquhart, Schuller, Menten, Bontemps, Herpin, Schilke, Beuther, Walmsley,
Motte, Garay, Zavagno
040-12
Polarization study of CN emission towards the massive
protostellar objects Cyg-N3 and Cyg-N63: How
strong is the role of the magnetic field in the cloud
fragmentation?
Herpin, Bontemps, Csengeri, Hezareh, Schneider, Wiesemeyer
041-12
A Study of the Pumping Mechanisms of SiO masers in
Evolved Stars
Cernicharo, Rizzo, Quintana, Dayou, Balanca, Godard, Velilla, Sánchez Contreras
042-12
Nucleosynthesis in AGB stars traced by isotopic ratios
Decin, Ramstedt, Olofsson, Daza, Milam
044-12
X-ray induced chemistry: systematic observations of
planetary nebulae
Bujarrabal, Kastner, Montez, Alcolea, Castro-Carrizo, Agundez, Santander-García, Balick
045-12
On the circumstellar envelopes of semi-regular longperiod variables
Alcolea, Bujarrabal, Castro-Carrizo
046-12
Spatially resolved chemistry around SNR IC 443
Martín Ruiz, Jimenez-Serra, Wesson, Aladro, Viti
047-12
TIME VARIABILITY OF MOLECULAR LINES IN IRC+10216
Cernicharo, Quintana-Lacaci, Guélin, Agúndez, Kahane, Teyssier, Pearson, Decin, De Beck, Barlow,
Garcia-Lario, Neufeld
048-12
G0.25+0.02: The Cradle of an Arches-like cluster?
Johnston, Beuther, Longmore, Rathborne, Ragan, Keto
049-12
2 mm Continuum Observations of the Galactic Center
Region
Staguhn, Kovács, Benford, Morris
050-12
Molecular gas in luminous M33 HII region complexes
Israel, Braine, Buchbender, Heiner
054-12
The gas-to-dust ratio in edge-on spiral galaxies
Allaert, Gentile, Baes, Verstappen
055-12
Low-metallicity star formation: where is the molecular
gas?
Lebouteiller, Cormier, Madden, Galliano, Hony, Bayet, Hughes, Barlow, Karczewski, Viti
056-12
Star formation laws and efficiency from the centre to
the outer edge of the XUV disk of the isolated galaxy
CIG 96
Scott, Leon, Montenegro-Verdes, Gil De Paz, Dobbs, Usero, Burillo
057-12
How Do Stars Form in Extragalactic Spiral Arms?
Topal, Bureau, Bayet, Yildiz, Davis, Ozeren, Yildiz, Etli
058-12
Mapping galactic disk breaks in CO
Munoz-Mateos, Leroy, Sheth
059-12
The Behaviour of Cold Gas in Damp-Mergers
Brassington, Duc, Belles, Lisenfeld, Brinks, Mundell
061-12
Chemical differentiation in the giant molecular halo
of M 82
González-García, García-Burillo, Fuente, Usero, Aladro, Abreu, Pilleri, Berné, Bayet
062-12
Unleashing the ISM chemistry in isolated galaxies
Martín, Verdes-Montenegro, Aladro, Espada, Kramer, Scott
063-12
Spectral Line Surveys toward Nearby Spiral Galaxy M51
in 3 mm Band
Yoshimasa, Sorai, Sakai, Yamamoto
064-12
A Complete Characterization of the Star-forming ISM in Bigiel, Schinnerer, Usero, Leroy, Gonzalez, Pety, Dumas, Hughes, Colombo, Garcia-Burillo
M51 with EMIR
065-12
Origin of the deviation from the LFIR-LHCN correlation
in the most isolated galaxies
067-12
Determining the Resolved Star Formation Law and Dust Dwek, Staguhn, Arendt, Eufrasio
Masses in NGC 6946
069-12
The gas content of high sSFR galaxies in the local
volume: implications for distant galaxies
Lehnert, Driel
070-12
CO and Star Formation in Gas-dominated Massive
Galaxies
Haynes, Huang, Giovanelli, Adams, Brinchmann, Chengalur, Hallenbeck, Hunt, Masters, Saintonge,
Spekkens
071-12
CO and Star Formation Efficiency in Mass-Selected
Major Mergers
Gao, Xu, Lisenfeld, Yun, Jarrett
072-12
Star formation efficiencies and XCO in intermediate
mass galaxies
Saintonge, Tacconi, Kauffmann, Kramer, Schiminovich, Buchbender, Catinella, Cortese, Fabello, Genzel,
Gracia-Carpio, Giovanelli, Haynes, Heckman, Moran, Schuster, Sternberg, Wang
073-12
The Role of Molecular Gas in Galaxy Disk Growth and
Evolution
Bigiel, Kauffmann, Usero, Saintonge, Gonzalez, Catinella, Wang, Jozsa, Serra
074-12
Using IRAM to Construct the First Detailed Timeline of
Early-Type Galaxy Evolution
Zabludoff, Shirley, Yang, Walter, Narayanan, Smith
075-12
Dust and molecular gas in Virgo star-forming dwarf
galaxies
Grossi, Corbelli, Hunt, Bianchi, Giovanardi, Magrini, Pappalardo, Madden, Bomans, Davies, Smith,
Bizzocchi, De Medeiros, Papaderos, De Looze, Verstappen, Garcia, Vlahakis
076-12
Molecular Gas and Nuclear Activity in Isolated, NonInteracting Luminous Infrared Galaxies
Iwasawa, Evans, Aalto, Frayer, Perez-Torres, Privon, Herrero-Illana, Surace, Kim, Mazzarella, Armus,
Stierwalt, Conway
077-12
Dense Gas in the HerCULES Sample
Weiss, van der Werf, Rosenberg, Greve, Downes, Papadopoulos, Walter, Aalto
078-12
The KS Law, Nitrogen Chemistry, and Nucleosynthesis
in Nearby Vigorously Star Forming Galaxies
Henkel, García-Burillo, Aalto, Papadopoulos, Zhang, Gao, Graciá-Carpio, Mühle, Asiri, Pérez-Beaupuits,
Mauersberger, Baan, Costagliola, Spaans, Ao
079-12
Understanding AGN feedback with gas chemistry in
NGC 1266
Davis, Bayet, Martín, Meier, Young, Alatalo, Crocker, Bureau, Blitz
Ocaña Flaquer, Scott, Leon, Martín, Verdes-Montenegro
54
Ident.
Title
Investigators
082-12
Testing the link between star formation and AGN
Dicken, Nesvadba, Boulanger, Lehnert, Combes, Tadhunter
083-12
Radio cores shedding light on molecular outflows
Dasyra, Combes
085-12
The variability of the intrinsic radio power of AGN in
cluster cores with GISMO
Edge, Hogan, Staguhn, Kovács, Benford, Hlavacek-Larrondo, Fabian, Salomé, Grainge
086-12
MAPI: Monitoring AGN with Polarimetry at the IRAM-30 Agudo, Thum, Gómez, Casadio, Molina, Marscher, Jorstad, Wiesemeyer
m
087-12
Coordinated cm to mm monitoring of variability and
spectral evolution of a selected it Fermi blazar sample
Fuhrmann, Zensus, Nestoras, Krichbaum, Angelakis, Schmidt, Karamanavis, Ungerechts, Sievers,
Readhead
089-12
Measuring the ISM content of optically luminous Type
2 QSOs
Petric, Ho, Omont, Billot
090-12
TANGO: Molecular gas content in radio galaxies at
medium redshift
Ocaña Flaquer, Leon, Verdes-Montenegro, Scott
091-12
CO Study for Dust-Rich Quasars at Intermediate
Redshifts
Dai, Bergeron, Omont, Elvis, Fazio, Huang, Hatziminaoglou, Perez-Fournon, Rigopoulou, Willmer
092-12
The molecular gas content of 0.2< z < 0.35 SDSS type
2 quasars.
Villar Martín, Colina, García-Burillo, Pérez-Torres, Rodríguez, De Breuck, Emonts, Humphrey, MartínezSansigre
093-12
Obtaining CO(1-0) and CO(2-1) for ULIRGs with mid and Spoon, Farrah, Afonso, Bernard-Salas, Borys, Clements, Connolly, Connolly, Cooray, Cormier, Efstathiou,
high-J CO measurements from Herschel-SPIRE-FTS
Lebouteiller, Oliver, Pearson, Rigopoulou, Roseboom, Rowan-Robinson, Surace, Verma, Wang, Wardlow,
Westmoquette
094-12
Bridging local and high-z ULIRGs; A detailed study of
the ISM in z~0.5 ULIRGs
Magdis, Rigopoulou, Cox, Herrero, Omont, Heywood, Oliver, Bock, Pearson, Farrah, Virdee, Huang,
Valtchanov
095-12
Search for a cosmological variation of the protonelectron mass ratio via methanol
Ubachs, Henkel, Bagdonaite, Menten
097-12
GISMO snapshots: Obtaining the flux at 2 mm of UltraRed Herschel Galaxies
Perez Fournon, Dannerbauer, Bertoldi, Omont, Riechers, Clements, Conley, Cox, Ivison, Michalowski
098-12
The GISMO 2 mm GDF: Pushing the Deepest (Sub-)
Millimeter Field To the Confusion Limit
Staguhn, Walter, Kovács, Benford, Decarli, Da Cunha
099-12
Disentagling SZ Clusters and Dusty Galaxies.
Kovács, Staguhn, Benford
102-12
CO Redshift Search for Exceptionally Bright Lensed
Herschel Sources
Kneib, Dessauges-Zavadsky, Boone, Combes, Omont, Egami, Rex, Rawle, Swinbank, Schaerer, Smail
103-12
Variation of Physical Constants: molecular absorption
at high z
Lattanzi, Combes, Petitjean, Salome
104-12
Extreme Star formation in five QSOs at z~4.8
Salomé, Combes, Dasyra
105-12
Ambipolar diffusion and magnetic fields in envelopes
of prestellar cores
Lippok, Launhardt, Li, Pavlyuchenkov, Stutz, Henning
106-12
Probing C18O in the envelope of the intermediate mass
(IM) protostar NGC 7129 FIRS 2
Fuente, Caselli, Mccoey, Cernicharo, Johnstone, Castro-Carrizo, Fich, Dishoeck, Kempen, Tisi, Alonso-Albi
111-12
Looking for embedded compact sources in cold,
massive clumps revealed by ATLASGAL
Csengeri, Wyrowski, Urquhart, Menten, Schuller, Bontemps
D01-12
Completing the chemical survey with the template
source Orion-KL (053-11)
Beuther, Gerner, Linz, Henning, Vasyunina, Semenov, Banerjee, Dullemond
PLATEAU DE BURE INTERFEROMETER
Ident.
Title of investigation
Authors
Q052
Deep study of the circumstellar envelopes of AGB &
early post-AGB stars
Castro-Carrizo, Alcolea, Bujarrabal, Grewing, Lindqvist, Lucas, Neri, Olofsson, Quintana-Lacaci, Schöier,
Winters
S0D7
Star Forming Histories and Gas Fractions of Galaxies
from z=1-3
Genzel, Tacconi, Davis, Bolatto, Bournaud, Burkert, Combes, Cooper, Cox, Schreiber, Garcia-Burillo,
Gracia-Carpio, Lutz, Naab, Neri, Omont, Shapiro, Shapley, Sternberg, Weiner
T0C5
The [CII]-forest: a new powerful tool for cosmology
Maiolino, Gallerani, Ferrara, Lutz, Genzel, Tacconi
T0CC
IRAM Lensing Survey: Probing Galaxy Formation in
the Early Universe
Kneib, Clément, Cuby, Peroux, Ilbert, Jablonka, Boone, Combes, Neri, Krips, Lagache, Beelen, Pello,
Courbin, Meylan, Schaerer, Dessauges, Knudsen, van der Werf, Richard, Smail, Swinbank, Chapman,
Ivison, Egami, Altieri, Valtchanov
U052
Class 0 protostars with PdBI: Solving the angular
momentum problem?
André, Maury, Testi, Launhardt, Codella, Cabrit, Gueth, Lefloch, Maret, Bottinelli, Bacmann, Belloche,
Bontemps, Hennebelle, Klessen, Dullemond
U09E
An Exploratory Redshift Survey in the Hubble Deep
Field North
Walter, Carilli, Daddi, Cox, Riechers, Decarli, Bertoldi, Weiss, Neri, Menten, Dannerbauer, Bell, Dickinson,
Ellis, Chiu, Krumholz, Robertson
U0DE
Physics of Gas and Star Formation in Galaxies at z=1.2 Tacconi, Combes, Genzel, Bolatto, Bournaud, Burkert, Cooper, Cox, Davis, Förster Schreiber, GarcíaBurillo, Graciá-Carpio, Lutz, Naab, Neri, Newman, Sternberg, Weiner
V--8
A high-resolution map in C[II] of HDF850.1. - A
possible example of a merger at z = 5.2
Cox, Neri, Walter, Downes, Krips
V--A
Influence of environment on cold gas in galaxies at
moderate redshift
Jablonka, Combes, Rines, Finn
Annual report 2012
55
Ident.
Authors
V--B
Confirming pure rotational emission from TiO and
TiO2 toward VY CMa
Menten, Kaminśki, Young, Patel, Gottlieb
V007
Revealing substructure in a very young starless core
in the Pipe Nebula
Girart, Frau, Palau, Padovani, Morata, Beltrán, Estalella
V021
Physical conditions in the interstellar medium of
early-type galaxies
Bureau, Topal, Bayet, Krips, Crocker, Young, Blitz, Combes, Davis, Alatalo, Cappellari, Emsellem, Krajnovic,
McDermid
V043
Continuum imaging of the brightest mm sources
from H-ATLAS
Bertoldi, Dannerbauer, Cox, Omont, Neri, Beelen, Negrello, Dunne, Verma, Ivison, Eales, Cooray, Glenn,
Michalowski, van der Werf, Bussmann, Riechers, de Zotti, Ibar
V04A
An efficient Program for Finding Lensed Galaxies at
z>4 - II
Krips, Cox, Dannerbauer, Eales, Omont, Beelen, Bertoldi, Dunne, Aretxaga, Hughes, Ivison, Cooray, Dye,
Frayer, Negrello, Smail
V053
The nucleus and inner coma of comet C/2009 P1
(Garradd)
Boissier, Bockelée-Morvan, Groussin, Biver, Crovisier, Moreno, Colom, Jorda, Lamy
V054
Mapping the D/H ratio in the Martian atmosphere
Fouchet, Moreno, Lellouch, Montmessin
V059
The origin of molecules in protostellar jets: a pilot
study of HH 111
Lefloch, Cabrit, Yvart, Gueth, Codella, Pineau des Forêts, Podio, Dougados
V05A
Nature of a candidate first protostellar core
discovered with Herschel & MAMBO
Maury, André, Könyves, Men’shchikov, Bontemps, Pezzuto, Testi, Ward-Thompson, Commerçon,
Hennebelle
V05B
Precise measurements of the deuteration of water in
low-mass protostars
Persson, Jørgensen, Dishoeck, Harsono
V060
Fragmentation and monolithic collapse to form
high-mass stars
Bontemps, Csengeri, Duarte-Cabral, Schneider, Motte, Gueth, Herpin, Bonnell, Commerçon, Hennebelle
V061
The fragmentation of massive dense cores detected
by Herschel
Hennemann, Motte, Csengeri, Schneider, Hill, Luong, Bontemps
V064
The Physical Structure of Embedded Disks
van Dishoeck, Harsono, Jørgensen, Hogerheijde, San Jose Garcia
V065
The innermost regions of high-mass accretion disks
Beuther, Linz, Henning
V06C
A complete homogeneous CO survey of northern FU Kóspál, Ábrahám, Hogerheijde, Brinch
Ori-type objects
V06E
UY Aurigae: a prototypical circumbinary disk?
Piétu, Tang, Dutrey, Guilloteau, Di Folco, Boehler, Gueth, Beck, Barry, Simon
V06F
Dust in low-weight disks: constraining models of
grain evolution
Testi, Benisty, Natta, Ricci, Birnstiel, Neri
V074
Masers and shocks in the gas around HVC stars
Quintana-Lacaci, Castro-Carrizo, Bujarrabal, Alcolea
V075
Testing the anion chemistry II: the case of CN-
Guélin, Cernicharo, Agundez, Winters, Thaddeus, Gottlieb, McCarthy
V077
The mass loss properties of the Red Supergiant stars
Quintana-Lacaci, Castro-Carrizo, Bujarrabal
V078
Molecular filament in the Crab Nebula
Salomé, Hily-Blant, Castro-Carrizo, Ferland, Combes, Baldwin, Loh, Fabian
V07E
Chemistry and environment of M 82 and IC 342: a
mapping survey
Henkel, Mauersberger, Martin, Aladro, Bayet, Viti, Wiklind, Peck, Vila-Vilaro, Sawada, Matsushita,
Papadopoulos
V085
Dense Molecular Gas around AGN
Davies, Sternberg, Graciá-Carpio, Mark, Orban de Xivry, Dodds-Eden
V086
Imaging the remarkable dense AGN wind from the
ULIRG Mrk231
Aalto, Garcia-Burillo, Costagliola, Muller, van der Werf, Henkel, Winters, Neri
V087
Towards a physical understanding of the massive
outflow in Mrk 231
Feruglio, Fiore, Maiolino, Piconcelli, Cicone, Krips, Chang, Aussel
V088
A new molecular outflow and/or streamer in
NGC6240
Feruglio, Fiore, Maiolino, Piconcelli, Cicone, Sturm, Davies
V08A
Cygnus A: AGN feedback and cooling flow
Casasola, Combes, Nakai, Salomé, Prandoni, Mignano, García-Burillo, Paladino, Hunt, Magrini, Rossetti
V08B
Mapping the HCN and HCO+ emission in NGC 1275
Salomé, Edge, Combes, Downes, Lim, Egami, Fabian, Johnstone, Oonk, Mittal, McNamara, Ferland,
Boulanger, Nesvadba
V08C
Resolving Molecular Outflows in LIRGs/ULIRGs: the
case of IRAS17208-0014
García-Burillo, Colina, Alonso-Herrero, Aalto, Combes, Canadas, Arribas, van der Werf, Villar-Martin,
Costagliola, Usero, Henkel, Hunt, Neri, Muller, Planesas
V094
The nature of the unique source SWIFT J1644+57
Guziy, Agudo, Castro-Tirado, Bremer, Winters, Gorosabel, Gómez, Sánchez-Ramirez, Tello
V095
First detections of molecular emission in damped
Lyman-α systems
Dessauges-Zavadsky, Kanekar, Fumagalli, Prochaska
V09A
The Molecular Component of a Massive Outflow at
z=1.2
Hailey-Dunsheath, Stacey, Brisbin, Nikola, Ferkinhoff
V09D
Searching for Molecular Gas in a Highly Amplified
Star-Forming Spiral Galaxy at z=1.49
Swinbank, Bower, Livermore, Richard, Smail
V09E
2 in 1: Gas fractions in a z = 1.4 elliptical & its
enigmatic neighbour
Sargent, Daddi, Onodera, Strazzullo, Dannerbauer, Bournaud, Martig
V0A2
Connecting QSOs and SMGs: Completing the sample. Smail, Swinbank, Simpson, Danielson, Cox, Bonfield, van der Werf, Jarvis, Coppin, Ivison, Hughes,
Vaccari, Dunlop, Verma, Clements, Leeuw, Smith
V0A3
Understanding the link between SMGs and ‘’main
sequence’’ star forming galaxies
Bothwell, Chapman, Genzel, Tacconi, Lutz, Greve, Bertoldi, Neri, Omont, Cox, Smail, Ivison, Biggs, Blain,
Casey, Muxlow, Beswick
V0A6
Understanding the Nature of Herschel-Selected
Submillimeter Galaxies
Riechers, Omont, Perez-Fournon, Cox, Cooray, Wardlow, Neri, Clements, Ivison, Bock, Oliver
56
Ident.
Authors
V0A7
Hi-res imaging of a uniquely bright sample of SMGs
- II
Cox, Ivison, Bertoldi, Omont, Fournon, Cooray, Eales, Frayer, Jarvis, Krips, Negrello, Neri, Smail, Swinbank,
van der Werf, Leeuw, Dannerbauer, Verma
V0A9
A Systematic Study of CO Excitation in High-Redshift
Quasar Host Galaxies
Riechers, Walter, Carilli, Neri, Cox, Weiss, Bertoldi
V0AA
The nature of star formation in merging-driven
starburts at z>2
Magdis, Daddi, Sargent, Dickinson, Strazzullo, Elbaz, Pannella, Galliano, Walter, Feruglio
V0B0
Identification of the highest redshift H-ATLAS and
HerMES galaxies
Bertoldi, Perez-Fournon, Omont, Dannerbauer, Lagache, Bethermin, Michalowski, Ivison, Clements,
Negrello, White, Benford, Temi, Vaccari, Riechers, Bock, Vieira, Cooray, Wardlow, Coppin, Frayer, DeZotti,
Massardi, Cava
V0B1
Exploring emission in high-z strongly lensed
Herschel galaxies
Omont, van der Werf, Neri, Cox, Krips, Riechers, Harris, Weiss, Gavazzi, Baker, Bertoldi, Beelen, Clements,
Cooray, Dannerbauer, Eales, Frayer, Guélin, Ivison, Lehnert, Lupu, Michalowski, Negrello, Leeuw
V0B2
A survey of ionized Nitrogen ([NII]) at high redshift.
Decarli, Walter, Maiolino, Carilli, Riechers, Bertoldi, Weiss, Cox, Neri
V0B3
Minor mergers and quasar feedback at z=4
Maiolino, Gallerani, Neri, Walter, Martin, de Breuck, Caselli, Krips, Meneghetti, Nagao, Wagg, Walmsley
V0B6
Faint CO Emitters in the Hubble Deep Field North
Walter, Carilli, Daddi, Cox, Riechers, Decarli, da Cunha, Bertoldi, Weiss, Neri, Elbaz, Menten, Dannerbauer,
Bell, Dickinson, Ellis, Chiu, Krumholz
V0B8
Comprehensive Study of an Exceptionally Bright
Lensed SMG at z~4.6
Boone, Combes, Egami, Omont, Dessauges-Zavadsky, Schaerer, Richard, Kneib, Smail, Swinbank, Edge,
Ivison, van der Werf, Rex, Rawle, Gurwell, Casey, Smith, Pham, Pello
V0B9
A first [CII] imaging survey of z>4 galaxies
Bertoldi, Knudsen, Walter, Riechers, Cox, Carilli, Wang, Maiolino, Omont, Weiss, Neri, Schinnerer
V0BA
Constraining the gas content of main sequence
galaxies at 4.4 < z < 5.6
Daddi, Sargent, Dickinson, Walter, Bournaud, Madden, Dekel, Dannerbauer, Elbaz, Magdis, Feruglio
V0BD
A Detailed Investigation of the ISM in the Most
Distant Starburst Galaxy
Riechers, Perez-Fournon, Omont, Cox, Bradford, Clements, Cooray, Wardlow, Neri, Krips, Dowell, Ivison,
Conley, Vieira, Bock, Oliver
V0BE
Nature and Excitation of Submillimeter H2O Emission
at z=6.42
Riechers, Weiss, Walter, Neri, van der Werf, Cox, Carilli, Bertoldi, Wang, Omont, Maiolino
V0C0
Atomic and Molecular Gas in a Spectroscopically
Confirmed Quasar Host Galaxy at z=7.1
Venemans, Walter, Decarli
V0C2
Unveiling the population of highly obscured and
high-z gamma-ray bursts (ToO)
Castro-Tirado, Bremer, Winters, Gorosabel, Guziy, de Ugarte Postigo, Pérez-Ramírez, Castro Cerón, Tello,
Sánchez-Ramírez
W--1
A likely z ~3 galaxy cluster detected with Planck,
Herschel, and Spitzer [DDT]
Dole, Nesvadba, König, Krips, Chary, Beelen, Flores-Cacho, Frye, Giard, Guery, Lagache, Montier, Omont,
Pointecouteau, Puget, Welikala, Yan
W--2
Luminous CO in bright Herschel-ATLAS galaxies at
z~3
Neri, Cox, Omont, Downes, Ivison, Krips
W--3
High-velocity molecular gas around SgrA*: feeding
the monster
Cernicharo, Lefloch
W--5
DDT proposal: Characterizing the ISM in a z~11
Galaxy
Walter, Riechers, Carilli, Decarli, Cox, Neri, Bertoldi, Weiss
W005
Outflow shocks traced in SiO: early hints for star
formation in IRDCs
Linz, Ragan, Beuther, Vasyunina, Schmiedeke
W009
Looking for embedded compact sources in cold,
massive clumps revealed by ATLASGAL
Csengeri, Wyrowski, Urquhart, Menten, Schuller, Bontemps
W00A
HDO and complex molecules in a deeply embedded
low-mass protostar
Persson, Jørgensen, Dishoeck, Harsono, Bisschop
W00B
Ambipolar diffusion and magnetic fields in envelopes Lippok, Launhardt, Li, Pavlyuchenkov, Stutz, Henning
of prestellar cores
W00D
Probing C18O in the envelope of the intermediate
mass (IM) protostar NGC 7129 FIRS 2
Fuente, Caselli, McCoey, Cernicharo, Johnstone, Castro-Carrizo, Fich, Dishoeck, Kempen, Tisi, AlonsoAlbi
W00F
Probing the expansion of a hypercompact HII region
Sánchez-Monge, Moscadelli, Cesaroni, Beltrán, Neri
W010
Investigating Molecular outflows in Brown Dwarfs
Dougados, Whelan, Monin, Lefloch, Alves, Cabrit
W013
Grain growth in transitional disks
Pinilla, Ricci, Benisty, Isella, Natta, Testi
W014
Constraining the evolution of solids in protoplanetary Ricci, Testi, Williams, Wilner, Neri
disks with the PdBI
W016
MaYS, Mass (and ages) of Young Stars: Dynamical
masses from CN(2-1)
White, Teixera, Palla, Chapillon
W018
Structure and excitation in the CSEs around C-stars
with high expansion velocity
Quintana-Lacaci, Castro-Carrizo, Bujarrabal, Alcolea
W019
Testing the anion chemistry in IRC+10216 (3): Where
is C4H-?
Guélin, Cernicharo, Agundez, Winters, Thaddeus, McCarthy
W01D
Peering into a site of cosmic rays acceleration
Ceccarelli, Hily-Blant, Vaupré
W01E
A cold gas reservoir to fuel M31 nuclear black hole
and stellar cluster
Melchior, Combes
W022
Mapping the molecular gas conditions in nearby
starburst galaxies
Rodríguez, Mühle, Aalto, Alberdi, Pérez-Torres
W026
Massive molecular outflows and negative feedback
in active galaxies
Sturm, Graciá-Carpio, Maiolino, González-Alfonso, Hailey-Dunsheath, Davies, Veilleux, Fischer, Feruglio,
Piconcelli, Fiore, Garcia-Burillo, Aalto, Cicone
W027
CO-to-H2 conversion factor in Mrk 231
Feruglio, Aalto, Maiolino, Sturm, Cicone, Fiore, Garcia-Carpio, Veilleux, Piconcelli, Garcia-Burillo, Bremer,
Winters, Aussel, Krips, Chang
Annual report 2012
Ident.
W028
Vibrationally excited HCN in Mrk231 - Probing the hot Aalto, Muller, Costalgiola, Garcia-Burillo, van der Werf, Winters, Henkel, Gonzalez-Alfonso, Neri
core and the nuclear outflow
W02B
A molecular outflow in the advanced merger NGC
1614
García-Burillo, Usero, Casznadas, Colina, Aalto, Alonso-Herrero, Combes, Hunt, Tacconi, Graciá-Carpio,
Neri, Planesas, Arribas
W02D
Monitoring periodic flux variations of 3C 66B
Iguchi, Okuda, Sudou, Matsuzawa, Yoshiike, Nagai
W02E
Agudo, Castro-Tirado, Guziy, Bremer, Winters, Gorosabel, Gómez, Sánchez-Ramirez, Tello
W032
The highest density starbursts in the Universe
Hickox, Geach, Diamond-Stanic, Moustakas, Robania, Rudnick, Tremonti
W034
The Interplay Between Feedback and Gas Supply at
Intermediate Redshift
Rubin, Decarli, Cucchiara, Walter, Hennawi, Prochaska, Fumagalli
W036
Deciphering the impact of the environment on cold
gas in cluster galaxies
Jablonka, Combes, Kneib, Jauzac, Egami, Haines, Pereira
W037
Galaxy Evolution and Star Formation Efficiency at 0.6
< z < 1.
Combes, García-Burillo, Braine, Schinnerer, Walter, Colina
W039
First mm observations of a massive black hole binary
candidate.
Decarli, Dotti, Volonteri, Walter
W03A
Feedback & Mergers in Luminous AGN at z=1.3
Rosario, Lutz, Genzel, Tacconi, Combes, Saintonge
57
Authors
W03E
Molecular Gas in a Galaxy Cluster at z = 1.4
Casasola, Magrini, Combes, Fontani, Mignano, Paladino, Sani
W03F
The Molecular Gas in High-z Star-Forming Galaxies
from HiZELS
Swinbank, Smail, Simpson, Sobral, Best, Geach, van der Werf
W041
First detection of CO in a high-z Compton-Thick QSO
Feruglio, Daddi, Fiore, Comastri, Elbaz, Alexander, Dickinson, Piconcelli, Gilli, Brusa, Vignali, Onodera,
Bournaud, Sargent, Pannella, Krips
W042
Measuring molecular gas in strongly lensed starforming galaxies
Dessauges-Zavadsky, Combes, Boone, Omont, Schaerer, Zamojski, Richard, Kneib, Egami, Rex, Rawle,
van der Werf, Péroux
W043
CO in high-z lensed galaxies with Herschel spectra
Nesvadba, Malhotra, Combes, Rhoads, Guerin, Lehnert, Frye
W044
Does AGN activity in galaxies correlate with their gas
content?
Mullaney, Daddi, Sargent, Juneau, Elbaz, Dickinson
W045
Herschel Extreme Starbursts at Redshift ~2
Rodighiero, Lutz, Tacconi, Genzel, Förster Schreiber, Wuyts, Popesso, Berta, Renzini, Cimatti, Gruppioni,
Zamorani, Andreani, Daddi, Carollo, Lilly, Onodera, Bschorr, Franceschini, Baronchelli, Lo, Faro, Silverman
W046
Confirming the membership of SMGs in the most
distant galaxy cluster
Dannerbauer, Daddi, Strazzullo, Gobat, Sargent, Carollo, Cimatti, Figoguenov, Onodera, Pannella,
Renzini, Ziegler
W04A
Understanding the Nature of Herschel-Selected
Submillimeter Galaxies
Riechers, Omont, Perez-Fournon, Neri, Cox, Cooray, Wardlow, Clements, Ivison, Magdis, Bock, Oliver
W04C
CO in the most overdense cluster known at z>2.
Chapman, Aravena, Smail, Steidel
W04D
Exploring the Cores of Lensed Herschel Galaxies
Using H2O Lines
Omont, van der Werf, Yang, Neri, Beelen, Krips, Ivison, Cox, Riechers, Harris, Weiss, Gavazzi, Baker,
Bertoldi, Bussmann, Cooray, Dannerbauer, Eales, Gao, Fu, Guélin, Lehnert, Lupu, Menten, Negrello
W04E
Revealing the Nature of Lyman-α Nebulae in the
Distant Universe
Yang, Walter, Decarli, Weiss, Bertoldi
W052
HerMES galaxies
Bertoldi, Perez-Fournon, Omont, Dannerbauer, Lagache, Bethermin, Michalowski, Ivison, Clements,
Negrello, White, Benford, Temi, Vaccari, Riechers, Bock, Vieira, Cooray, Wardlow, Coppin, Frayer, DeZotti
W053
Small-scale structure of molecular gas at z=5.243
Boone, Combes, Richard, Egami, Rex, Rawle, Smail, Ivison, Omont, Dessauges-Zavadsky, Schaerer, van
der Werf, Pham
W054
A systematic search for CO in a flux limited sample of
z=6 quasars
Venemans, Walter, Decarli
W056
Exploring the Unusual CO and H2O Excitation of z~6
Quasars
Riechers, Neri, Walter, Carilli, Wang, Cox, Weiss, Bertoldi, Omont, van der Werf, Fan, Maiolino
W058
A Detailed Investigation of the ISM in the Most
Distant Starburst Galaxy
Riechers, Perez-Fournon, Omont, Neri, Cox, Bradford, Clements, Cooray, Wardlow, Krips, Dowell, Ivison,
Kamenetzky, Conley, Vieira, Bock, Oliver
W059
Mapping a quasar-driven massive outflow in the
early Universe
Maiolino, Gallerani, Neri, Cicone, Ferrara, Genzel, Lutz, Sturm, Tacconi, Walter, Feruglio, Fiore, Pinconcelli
W05A
Blind redshifts for ultra-red Herschel galaxies
Krips, Ivison, Bertoldi, Omont, Cox, Neri, Koenig, van der Werf, Dannerbauer, Eales, Valiante, Clements,
Swinbank
W05E
Castro-Tirado, Bremer, Winters, Gorosabel, Guziy, De Ugarte Postigo, Pérez-Ramírez, Castro Cerón, Tello,
Sánchez-Ramírez
W061
First high resolution mapping of C3H+ in the ISM
Guzmán, Pety, Gratier, Goicoechea, Gerin
W069
Imaging the spectral signature of a protostellar
J-shock
Codella, Gueth, Benedettini, Busquet, Cabrit, Ceccarelli, Lefloch, Nisini, Gómez-Ruiz
W075
How much water in the protoplanetary disk of
DG-Tau
Podio, Codella, Cabrit, Kamp, Nisini, Dougados, Gueth, Bacciotti
W09C
Agudo, Castro-Tirado, Guziy, Bremer, Winters, Gorosabel, Gómez, Sánchez-Ramirez, Tello
W0AC
Building Up CO Ladders in Lyman-α Blobs
Yang, Walter, Decarli, Weiss, Bertoldi
W0AD
Resolving the morphology of the first WISE-identified Blain, Benford, Bridge, Eisenhardt, Jones, Yan, Tsai, Wu
ULIRG
W0B4
Probing the Excitation of H2O in Lensed Herschel
Galaxies
Omont, van der Werf, Yang, Neri, Beelen, Krips, Ivison, Cox, Riechers, Harris, Weiss, Gavazzi, Spaans, Baker,
Bertoldi, Bussmann, Dannerbauer, Downes, Eales, Gao, Fu, Guélin, Lehnert, Lupu, Menten, Michalowski,
Negrello, Temi, Valiante
58
Ident.
Authors
W0B7
Ionized Nitrogen ([NII]) at high redshift
Decarli, Walter, Maiolino, Carilli, Riechers, Bertoldi, Weiss, Cox, Neri
W0BD
HerMES galaxies
Bertoldi, Perez Fournon, Omont, Dannerbauer, Lagache, Bethermin, Michalowski, Ivison, Clements,
Negrello, White, Benford, Temi, Vaccari, Riechers, Bock, Vieira, Cooray, Wardlow, Coppin, Frayer, DeZotti,
Massardi, Cava, Smail, Swinbank, Bremer, Verma, Rigopoulou, Aretxaga, Hughes, Marrone, van Kampen,
Eales, van der Werf, Bussmann, Conley, Oliver, Valiante
W0C3
A Quasar-Starburst Merger System at the Epoch of
Reionization?
Wang, Carilli, Neri, Walter, Riechers, Fan, Willott, Cox, Bertoldi, Omont, Menten, Strauss, Wagg
W0CA
Castro-Tirado, Bremer, Winters, Gorosabel, Guziy, Pérez-Ramírez, Castro Cerón, Tello, Sánchez-Ramírez
Annual report 2012
59
Annex II – Publications in 2012
the list of refereed publications, conferences and workshop papers as well as thesis based upon data
obtained using the IRAM instruments are provided in the following two tables : the first table gives the
publications with the IRAM staff members as co-author (including technical publications by the IRAM staff ),
and the second table those with results from the user’s community.
The running number is the cumulative number since the first annual report was published for the year 1987.
2012 PUBLICATION LIST: IRAM (CO)AUTHORS :
1651
Faint high-redshift AGN in the Chandra
deep field south: the evolution of the
AGN luminosity function and black hole
demography
Fiore F., Puccetti S., Grazian A., Menci N., Shankar F., Santini P., Piconcelli E., Koekemoer A. M.,
Fontana A., Boutsia K., Castellano M., Lamastra A., Malacaria C., Feruglio C., Mathur S., Miller N.,
Pannella M.
A&A 537, A16
1652
Detection of HCN, HCO+, and HNC in
the Mrk 231 molecular outflow. Dense
molecular gas in the AGN wind
Aalto S., Garcia-Burillo S., Muller S., Winters J. M., van der Werf P., Henkel C., Costagliola F., Neri R. A&A 537, A44
1653
Chemistry in disks. VI. CN and HCN in
protoplanetary disks
Chapillon E., Guilloteau S., Dutrey A., Piétu V., Guélin M.
A&A 537, A60
1654
The Herschel M 33 extended survey
(HerM33es): PACS spectroscopy of the star
forming region BCLMP 302 (Corrigendum)
Mookerjea B., Kramer C., Buchbender C., Boquien M., Verley S., Relaño M., Quintana-Lacaci G.,
Aalto S., Braine J., Calzetti D., Combes F., Garcia-Burillo S., Gratier P., Henkel C., Israel F., Lord S.,
Nikola T., Röllig M., Stacey G., Tabatabaei F. S., van der Tak F., van der Werf P.
A&A 537, 3
1655
Pre-ALMA observations of GRBs in the mm/ de Ugarte Postigo A., Lundgren A., Martìn S., Garcia-Appadoo D., de Gregorio Monsalvo I., Peck A&A 538, A44
submm range
A., MichaŃowski M. J., Thöne C. C., Campana S., Gorosabel J., Tanvir N. R., Wiersema K., CastroTirado A. J., Schulze S., De Breuck C., Petitpas G., Hjorth J., Jakobsson P., Covino S., Fynbo J. P. U.,
Winters J. M., Bremer M., Levan A. J., Llorente A., Sánchez-Ramìrez R., Tello J. C., Salvaterra R.
1656
The EMIR multi-band mm-wave receiver for Carter M., Lazareff B., Maier D., Chenu J.-Y., Fontana A.-L., Bortolotti Y., Boucher C., Navarrini A.,
the IRAM 30-m telescope
Blanchet S., Greve A., John D., Kramer C., Morel F., Navarro S., Peñalver J., Schuster K. F., Thum C.
1657
Dust and gas power spectrum in M 33
(HERM33ES)
Combes F., Boquien M., Kramer C., Xilouris E. M., Bertoldi F., Braine J., Buchbender C., Calzetti
D., Gratier P., Israel F., Koribalski B., Lord S., Quintana-Lacaci G., Relaño M., Röllig M., Stacey G.,
Tabatabaei F. S., Tilanus R. P. J., van der Tak F., van der Werf P., Verley S.
A&A 539, A67
1658
Ammonia and other parent molecules in
comet 10P/Tempel 2 from Herschel/HIFI
and ground-based radio observations
Biver N., Crovisier J., Bockelée-Morvan D., Szutowicz S., Lis D. C., Hartogh P., de Val-Borro M.,
Moreno R., Boissier J., Kidger M., Küppers M., Paubert G., Dello Russo N., Vervack R., Weaver H.
A&A 539, A68
1659
On the physical structure of IRC +10216.
Ground-based and Herschel observations
of CO and C2H
De Beck E., Lombaert R., Agúndez M., Daniel F., Decin L., Cernicharo J., Müller H. S. P., Min M.,
Royer P., Vandenbussche B., de Koter A., Waters L. B. F. M., Groenewegen M. A. T., Barlow M. J.,
Guélin M., Kahane C., Pearson J. C., Encrenaz P., Szczerba R., Schmidt M. R.
A&A 539, A108
1660
The first IRAM/PdBI polarimetric millimeter
survey of active galactic nuclei. II. Activity
and properties of individual sources
Trippe S., Neri R., Krips M., Castro-Carrizo A., Bremer M., Piétu V., Winters J. M.
A&A 540, A74
1661
Imaging diffuse clouds: bright and dark gas Liszt H. S., Pety J.
mapped in CO
1662
3C 286: a bright, compact, stable, and
highly polarized calibrator for millimeterwavelength observations
Agudo I., Thum C., Wiesemeyer H., Molina S. N., Casadio C., Gómez J. L., Emmanoulopoulos D.
1663
Simultaneous Planck, Swift, and Fermi
observations of X-ray and X-ray selected
blazars
Giommi P., Polenta G., Lähteenmäki A., Thompson D. J., Capalbi M., Cutini S., Gasparrini
A&A 541, A160
D., González-Nuevo J., León-Tavares J., López-Caniego M., Mazziotta M. N., Monte C., Perri
M., Rainò S., Tosti G., Tramacere A., Verrecchia F., Aller H. D., Aller M. F., Angelakis E., Bastieri
D., Berdyugin A., Bonaldi A., Bonavera L., Burigana C., Burrows D. N., Buson S., Cavazzuti E.,
Chincarini G., Colafrancesco S., Costamante L., Cuttaia F., D’Ammando F., de Zotti G., Frailis
M., Fuhrmann L., Galeotta S., Gargano F., Gehrels N., Giglietto N., Giordano F., Giroletti M.,
Keihänen E., King O., Krichbaum T. P., Lasenby A., Lavonen N., Lawrence C. R., Leto C., Lindfors E.,
Mandolesi N., Massardi M., Max-Moerbeck W., Michelson P. F., Mingaliev M., Natoli P., Nestoras I.,
Nieppola E., Nilsson K., Partridge B., Pavlidou V., Pearson T. J., Procopio P., Rachen J. P., Readhead
A., Reeves R., Reimer A., Reinthal R., Ricciardi S., Richards J., Riquelme D., Saarinen J., Sajina A.,
Sandri M., Savolainen P., Sievers A., Sillanpää A., Sotnikova Y., Stevenson M., Tagliaferri G., Takalo
L., Tammi J., Tavagnacco D., Terenzi L., Toffolatti L., Tornikoski M., Trigilio C., Turunen M., Umana
G., Ungerechts H., Villa F., Wu J., Zacchei A., Zensus J. A., Zhou X.
1664
Herschel/HIFI observation of highly excited Daniel F., Agúndez M., Cernicharo J., De Beck E., Lombaert R., Decin L., Kahane C., Guélin M.,
rotational lines of HNC toward IRC +10 216 Müller H. S. P.
A&A 542, A37
1665
On the calibration of full-polarization 86
GHz global VLBI observations
Martì-Vidal I., Krichbaum T. P., Marscher A., Alef W., Bertarini A., Bach U., Schinzel F. K., Rottmann
H., Anderson J. M., Zensus J. A., Bremer M., Sanchez S., Lindqvist M., Mujunen A.
A&A 542, A107
1666
Giant molecular clouds in the Local Group
galaxy M 33*
Gratier P., Braine J., Rodriguez-Fernandez N. J., Schuster K. F., Kramer C., Corbelli E., Combes F.,
Brouillet N., van der Werf P. P., Röllig M.
A&A 542, A108
1667
The structure of hot gas in Cepheus B
Mookerjea B., Ossenkopf V., Ricken O., Güsten R., Graf U. U., Jacobs K., Kramer C., Simon R.,
Stutzki J.
A&A 542, L17
A&A 538, A89
A&A 541, A58
A&A 541, A111
60
1668
Spectral line survey of the ultracompact HII Ginard D., González-Garcìa M., Fuente A., Cernicharo J., Alonso-Albi T., Pilleri P., Gerin M., Garcìa- A&A 543, A27
region Monoceros R2
Burillo S., Ossenkopf V., Rizzo J. R., Kramer C., Goicoechea J. R., Pety J., Berné O., Joblin C.
1669
Molecular abundances in the inner layers
of IRC +10216
Agúndez M., Fonfrìa J. P., Cernicharo J., Kahane C., Daniel F., Guélin M.
A&A 543, A48
1670
Cool and warm dust emission from M 33
(HerM33es)
Xilouris E. M., Tabatabaei F. S., Boquien M., Kramer C., Buchbender C., Bertoldi F., Anderl S.,
Braine J., Verley S., Relaño M., Quintana-Lacaci G., Akras S., Beck R., Calzetti D., Combes F.,
Gonzalez M., Gratier P., Henkel C., Israel F., Koribalski B., Lord S., Mookerjea B., Rosolowsky E.,
Stacey G., Tilanus R. P. J., van der Tak F., van der Werf P.
A&A 543, A74
1671
The physics and the structure of the
quasar-driven outflow in Mrk 231
Cicone C., Feruglio C., Maiolino R., Fiore F., Piconcelli E., Menci N., Aussel H., Sturm E.
A&A 543, A99
1672
Resolved [CII] emission in a lensed quasar
at z = 4.4
Gallerani S., Neri R., Maiolino R., Martìn S., De Breuck C., Walter F., Caselli P., Krips M., Meneghetti
M., Nagao T., Wagg J., Walmsley M.
A&A 543, A114
1673
The IRAM-30m line survey of the
Horsehead PDR. I. CF+ as a tracer of C+ and
as a measure of the fluorine abundance
Guzmán V., Pety J., Gratier P., Goicoechea J. R., Gerin M., Roueff E., Teyssier D.
A&A 543, L1
1674
Spectrally resolved C II emission in M
33 (HerM33es). Physical conditions and
kinematics around BCLMP 691
Braine J., Gratier P., Kramer C., Israel F. P., van der Tak F., Mookerjea B., Boquien M., Tabatabaei F.,
van der Werf P., Henkel C.
A&A 544, A55
1675
CN Zeeman observations of the NGC 2264- Maury A. J., Wiesemeyer H., Thum C.
C protocluster
A&A 544, A69
1676
Submillimeter line emission from LMC 30
Doradus: The impact of a starburst on a
low-metallicity environment
Pineda J. L., Mizuno N., Röllig M., Stutzki J., Kramer C., Klein U., Rubio M., Kawamura A.,
Minamidani T., Benz A., Burton M., Fukui Y., Koo B.-C., Onishi T.
A&A 544, A84
1677
Herschel/HIFI observations of CO, H2O and
NH3 in Monoceros R2
Pilleri P., Fuente A., Cernicharo J., Ossenkopf V., Berné O., Gerin M., Pety J., Goicoechea J. R., Rizzo A&A 544, A110
J. R., Montillaud J., González-Garcìa M., Joblin C., Le Bourlot J., Le Petit F., Kramer C.
1678
Two short mass-loss events that unveil
the binary heart of Minkowski’s Butterfly
Nebula
Castro-Carrizo A., Neri R., Bujarrabal V., Chesneau O., Cox P., Bachiller R.
1679
Variability of the blazar 4C 38.41 (B3
1633+382) from GHz frequencies to GeV
energies
Raiteri C. M., Villata M., Smith P. S., Larionov V. M., Acosta-Pulido J. A., Aller M. F., D’Ammando
A&A 545, A48
F., Gurwell M. A., Jorstad S. G., Joshi M., Kurtanidze O. M., Lähteenmäki A., Mirzaqulov D. O.,
Agudo I., Aller H. D., Arévalo M. J., Arkharov A. A., Bach U., Benìtez E., Berdyugin A., Blinov D. A.,
Blumenthal K., Buemi C. S., Bueno A., Carleton T. M., Carnerero M. I., Carosati D., Casadio C.,
Chen W. P., Di Paola A., Dolci M., Efimova N. V., Ehgamberdiev S. A., Gómez J. L., González A. I.,
Hagen-Thorn V. A., Heidt J., Hiriart D., Holikov S., Konstantinova T. S., Kopatskaya E. N., Koptelova
E., Kurtanidze S. O., Larionova E. G., Larionova L. V., León-Tavares J., Leto P., Lin H. C., Lindfors E.,
Marscher A. P., McHardy I. M., Molina S. N., Morozova D. A., Mujica R., Nikolashvili M. G., Nilsson
K., Ovcharov E. P., Panwar N., Pasanen M., Puerto-Gimenez I., Reinthal R., Richter G. M., Ros J. A.,
Sakamoto T., Schwartz R. D., Sillanpää A., Smith N., Takalo L. O., Tammi J., Taylor B., Thum C.,
Tornikoski M., Trigilio C., Troitsky I. S., Umana G., Valcheva A. T., Wehrle A. E.
1680
BR1202-0725: an extreme multiple merger
at z = 4.7
Salomé P., Guélin M., Downes D., Cox P., Guilloteau S., Omont A., Gavazzi R., Neri R.
A&A 545, A57
1681
Herschel/HIFI observations of red
supergiants and yellow hypergiants. I.
Molecular inventory
Teyssier D., Quintana-Lacaci G., Marston A. P., Bujarrabal V., Alcolea J., Cernicharo J., Decin L.,
Dominik C., Justtanont K., de Koter A., Melnick G., Menten K. M., Neufeld D. A., Olofsson H.,
Planesas P., Schmidt M., Soria-Ruiz R., Schöier F. L., Szczerba R., Waters L. B. F. M.
A&A 545, A99
1682
Winds of change - a molecular outflow in
NGC 1377? The anatomy of an extreme
FIR-excess galaxy
Aalto S., Muller S., Sakamoto K., Gallagher J. S., Martìn S., Costagliola F.
A&A 546, A68
1683
The circumstellar disk of AB Aurigae:
evidence for envelope accretion at late
stages of star formation?
Tang Y.-W., Guilloteau S., Piétu V., Dutrey A., Ohashi N., Ho P. T. P.
A&A 547, A84
1684
Millimeter imaging of submillimeter
galaxies in the COSMOS field: redshift
distribution
Smolčić V., Aravena M., Navarrete F., Schinnerer E., Riechers D. A., Bertoldi F., Feruglio C.,
Finoguenov A., Salvato M., Sargent M., McCracken H. J., Albrecht M., Karim A., Capak P., Carilli
C. L., Cappelluti N., Elvis M., Ilbert O., Kartaltepe J., Lilly S., Sanders D., Sheth K., Scoville N. Z.,
Taniguchi Y.
A&A 548, A4
1685
A detailed view of a molecular cloud in
the far outer disk of M 33. Molecular cloud
formation in M 33
Braine J., Gratier P., Contreras Y., Schuster K. F., Brouillet N.
A&A 548, A52
1686
The IRAM-30 m line survey of the
Horsehead PDR. II. First detection of the
l-C3H+ hydrocarbon cation
Pety J., Gratier P., Guzmán V., Roueff E., Gerin M., Goicoechea J. R., Bardeau S., Sievers A., Le Petit
F., Le Bourlot J., Belloche A., Talbi D.
A&A 548, A68
1687
Chemistry in disks. VIII. The CS molecule as
an analytic tracer of turbulence in disks
Guilloteau S., Dutrey A., Wakelam V., Hersant F., Semenov D., Chapillon E., Henning T., Piétu V.
A&A 548, A70
1688
The hyperfine structure in the rotational
spectrum of CF+
Guzmán V., Roueff E., Gauss J., Pety J., Gratier P., Goicoechea J. R., Gerin M., Teyssier D.
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High SiO abundance in the HH212
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First Detection of Hydrogen Chloride
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Constraining Dust and Molecular Gas
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The Metallicity Dependence of the CO ⟶
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Molecular Gas in Infrared Ultraluminous
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Multi-wavelength Observations of Blazar
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Detection of Atomic Carbon [C II] 158 mm
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Evidence for Low Extinction in Actively
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On the Variations of Fundamental
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The Impact of Interactions, Bars, Bulges,
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The ATLAS3D project - XI. Dense molecular
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Discovery of a detached H I gas shell
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Physical properties of dense molecular gas
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Evidence of strong quasar feedback in the
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The intense starburst HDF850.1 in a galaxy
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The GISMO-2 bolometer camera
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The Chemical Structure of Orion KL: A 2D
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Dense molecular gas around AGN: HCN/CO
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Bruni G., Mack K.-H., Dallacasa D., Montenegro-Montes F. M., Benn C. R., Carballo R., GonzálezSerrano J. I., Holt J., Jiménez-Luján F.
J. of Physics Conf.
Series 372, 012031
1767
Chemical complexity in NGC 1068
Aladro R., Viti S., Riquelme D., Martìn S., Mauersberger R., Martìn-Pintado J., Bayet E.
J. of Physics Conf.
Series 372, 012039
1768
10 pc Scale Circumnuclear Molecular Gas
Imaging of Nearby AGNs
Matsushita S.
J. of Physics Conf.
Series 372, 012043
1769
The feeding of activity in galaxies: a
molecular line perspective
Garcìa-Burillo S., Combes F.
J. of Physics Conf.
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1770
Molecular gas in active environments
Mühle S., Henkel C., de Maio T., Seaquist E. R.
J. of Physics Conf.
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1771
CI, [CII] and CO observations towards TNJ
1338-1942: Probing the ISM in a massive
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J. of Physics Conf.
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a Confusion Limited Spectral Survey of
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Cernicharo J., Tercero B., Marcelino N., Bell T., Palau A.
67th Internat.
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1773
The star-forming core ahead of HH 80N:
studying the interaction with a parsec
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Masqué Saumell J.-M.
PhDT
1774
Water deuteration in star-forming regions : Coutens A.
Contribution of Herschel/HIFI spectroscopic
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PhDT
1775
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Arzoumanian D., André P., Peretto N., Könyves V., Schneider N., Didelon P., Palmeirim P.
Symp. Proceedings
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1776
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by Herschel
Stutz A. M., Tobin J., Fischer W., S. T. Megeath, Stanke T., Ali B., Henning T.
Symp. Proceedings
of “from Atoms to
view of Star and
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1777
F-GAMMA program: Unification and
physical interpretation of the radio spectra
variability patterns in Fermi blazars and
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Angelakis E.
Proc of the 10th
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Mathews G.
AAS 219, #327.04
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Guillard P., Boulanger F., Appleton P., Falgarone E., Gusdorf A., Lisenfeld U., Duc P.
AAS 220, #333.13
1780
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acetonitrile and acetonitrile/acetylene ices
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Dawley M. M., McLain J., Abbott H. L., Orlando T. M.
American Geophys.
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68
Annex III – Committee members
EXECUTIVE COUNCIL
R. Bachiller, OAN-IGN, Spain
S. Guilloteau, Obs. Bordeaux, France
A. Barcia Cancio, CAY, Spain
J.M. Hameury, CNRS-INSU, France
R. Genzel, MPE, Germany
K. Menten, MPIfR, Germany
J. Gomez-Gonzalez, IGN, Spain
J.L. Puget, IAS, France
M. Schleier, MPG, Germany
SCIENTIFIC ADVISORY COMMITTEE
Ph. André, CEA, France
L. Tacconi, MPE, Germany
F. Boulanger, IAS, France
M. Tafalla, OAN-IGN, Spain
D. Jaffe, University of Texas, USA
P. de Vicente, OAN-IGN, Spain
R. Moreno, Obs. de Paris, France
D. Muders, MPIfR, Germany
F. Wyrowski, MPIfR, Germany
PROGRAM COMMITTEE
H. Beuther, MPIA, Germany
S. Garcia-Burillo, OAN-IGN, Spain
A. Blain, University of Leicester, UK
J. Goicoechea, CSIC/INTA, Spain
S. Bontemps, Obs. Bordeaux, France
C. Henkel, MPIfR, Spain
V. Bujarrabal, OAN-IGN, Spain
B. Lefloch, IPAG, France
C. Codella, INAF, Italy
E. Sturm, MPE, Germany
R. Dave, Steward Observatory, USA
C. Vastel, IRAP, France
H. Dole, IAS, France
AUDIT COMMISSION
Mr. Adams, CNRS, France
Mrs. Keil, MPG, Germany
Mrs. Maar, MPG, Germany
IRAM
6 x 15-meter interferometer, Plateau de Bure
Institut de Radioastronomie Millimétrique 30-meter diameter telescope, Pico Veleta
The Institut de Radioastronomie Millimétrique (IRAM) is a multi-national
scientific institute covering all aspects of radio astronomy at millimeter
wavelengths: the operation of two high-altitude observatories – a
30-meter diameter telescope on Pico Veleta in the Sierra Nevada (southern
Spain), and an interferometer of six 15 meter diameter telescopes on the
Plateau de Bure in the French Alps – the development of telescopes and
instrumentation, radio astronomical observations and their interpretation.
IRAM Addresses:
Institut de Radioastronomie
Millimétrique
300 rue de la piscine,
Saint-Martin d’Hères
F-38406 France
Tel: +33 [0]4 76 82 49 00
Fax: +33 [0]4 76 51 59 38
[email protected] www.iram.fr
Observatoire
du Plateau de Bure
Saint-Etienne-en-Dévoluy
F-05250 France
Tel: +33 [0]4 92 52 53 60
Fax: +33 [0]4 92 52 53 61
Avenida Divina Pastora 7, Local 20,
E-18012 Granada, España
Tel: +34 958 80 54 54
Fax: +34 958 22 23 63
[email protected]
Observatorio
Radioastronómico
de Pico Veleta
Sierra Nevada,
Granada, España
Tel: +34 958 48 20 02
Fax: +34 958 48 11 49
Designed and produced by rebusparis.com
Printed in France
The technical and scientific staff of IRAM develops instrumentation and
software for the specific needs of millimeter radioastronomy and for the
benefit of the astronomical community. IRAM’s laboratories also supply
devices to several European partners, including for the ALMA project.
IRAM’s scientists conduct forefront research in several domains of
astrophysics, from nearby star-forming regions to objects at cosmological
distances.
IRAM Partner Organizations:
Centre National de la Recherche Scientifique (CNRS) – Paris, France
Max-Planck-Gesellschaft (MPG) – München, Deutschland
Instituto Geografico Nacional (IGN) – Madrid, España
Annual Report 2012
Instituto de Radioastronomía
Milimétrica
IRAM was founded in 1979 by two national research organizations: the
CNRS and the Max-Planck-Gesellschaft – the Spanish Instituto Geográfico
Nacional, initially an associate member, became a full member in 1990.
Front Cover
Cas A as seen in the 2mm
wavelength band by NIKA (NEEL
IRAM KID ARRAY), the prototype
continuum camera at the 30m
telescope using lumped Element
Kinetic Inductance Detectors. The
emission from Cas A, a well known
supernova remnant, is dominated in
this band by synchrotron radiation.

IRAM Annual Report 2012

Transcription

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